u/erica/FinalBEpaper: erica.bib

@article{nobody3008,
        abstract = {},
        author = {},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
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        title = {},
        url = {},
        volume = {},
        year = {}
}
@article{alves2001,
        author = {{Alves}, J. F. and {Lada}, C. J. and {Lada}, E. A. },
        journal = {nature},
        month = jan,
        pages = {159-161},
        title = "{Internal structure of a cold dark molecular cloud inferred from the extinction of background starlight}",
        url = {http://adsabs.harvard.edu/abs/2001Natur.409..159A},
        volume = {409},
        year = {2001}
}
@ARTICLE{shu1977,
   author = {{Shu}, F. H.},
    title = "{Self-similar collapse of isothermal spheres and star formation}",
  journal = {\apj},
 keywords = {hydrodynamics, stars: formation },
     year = 1977,
    month = jun,
   volume = 214,
    pages = {488-497},
      doi = {10.1086/155274},
   adsurl = {http://adsabs.harvard.edu/abs/1977ApJ...214..488S},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}

}
@ARTICLE{teixeira2005,
   author = {{Teixeira}, P.S. and {Lada}, C.J. and {Alves}, J.F.},
    title = "{From dusty filaments to cores to stars: an infrared extinction study of lupus 3}",
  journal = {\apj},
     year = 2005,
    month = aug,
   volume = 629,
    pages = {276-287},
      doi = {10.1086/430849},
   adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...629..276T},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}


}
@ARTICLE{whitworth1985,
   author = {{Whitworth}, A. and {Summers}, D.},
    title = "{Self-similar condensation of spherically symmetric self-gravitating isothermal gas clouds}",
  journal = {\mnras},
 keywords = {computational astrophysics, condensing, gas flow},
     year = 1985,
    month = may,
   volume = 214,
    pages = {1-25},
   adsurl = {http://adsabs.harvard.edu/abs/1985MNRAS.214....1W},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{whitworth1996,
   author = {{Whitworth}, A.P. and {Bhattal}, A.S. and {Francis}, N. and {Watkins}, S.J.},
    title = "{Star formation and the singular isothermal sphere}",
  journal = {\mnras},
 keywords = {stars: formation },
     year = 1996,
    month = dec,
   volume = 283,
    pages = {1061-1070},
   adsurl = {http://adsabs.harvard.edu/abs/1996MNRAS.283.1061W},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}

}
@INPROCEEDINGS{shu1987,
   author = {{Shu}, F. H. and {Lizano}, S. and {Adams}, F.C.},
    title = "{Star formation in molecular cloud cores}",
  booktitle = "{Star forming regions; Proceedings of the Symposium, Tokyo, Japan}",
     year = 1987,
    pages = {417-433},
   adsurl = {http://adsabs.harvard.edu/abs/1987IAUS..115..417S},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{hunter1977,
   author = {{Hunter}, C.},
    title = "{The collapse of unstable isothermal spheres}",
  journal = {\apj},
     year = 1977,
    month = dec,
   volume = 218,
    pages = {834-845},
      doi = {10.1086/155739},
   adsurl = {http://adsabs.harvard.edu/abs/1977ApJ...218..834H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@INPROCEEDINGS{adams1987,
   author = {{Shu}, F. H. and {Adams}, F.C.},
    title = "{Star formation and the circumstellar matter of young stellar objects}", 
booktitle = {Circumstellar matter; Proceedings of the IAU Symposium, Heidelberg},
     year = 1987,
    month = jun,
    pages = {7-22},
   adsurl = {http://adsabs.harvard.edu/abs/1987IAUS..122....7S},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@INPROCEEDINGS{foster1994,
   author = {{Foster}, P.},
    title = "{A guide to isothermal gravitational collapse}",
booktitle = {Proceedings of the 4th Haystack Observatory Conference},
      year = 1994,
    month = may,
   volume = 65,
    pages = {105},
   adsurl = {http://adsabs.harvard.edu/abs/1994ASPC...65..105F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{anathpindika2013,
   author = {{Anathpindika}, S. and {Di Francesco}, J.D.},
    title = "{Does a prestellar core always become protostellar? Tracing the evolution of cores from the prestellar to protostellar phase}",
  journal = {\mnras},
 keywords = {hydrodynamics, stars: formation },
     year = 2013,
    month = apr,
   volume = 430,
    pages = {154-1866},
      doi = {10.1086/155274},
   adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.430.1854A},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{larson1969,
   author = {{Larson}, R.B.},
    title = "{Numerical calculations of collapsing protostar}",
  journal = {\mnras},
 keywords = {hydrodynamics, stars: formation },
     year = 1969,
    month = jan,
   volume = 145,
    pages = {271},
      doi = {10.1086/155274},
   adsurl = {http://adsabs.harvard.edu/abs/1969MNRAS.145..271L},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{penston1969,
   author = {{Penston}, M.V.},
    title = "{Dynamics of self-gravitating spheres - III. Analytical results in the free-fall of isothermal cases}",
  journal = {\mnras},
     year = 1969,
    month = jan,
   volume = 144,
    pages = {425},
   adsurl = {http://adsabs.harvard.edu/abs/1969MNRAS.144..425P},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{myers2008,
 author = {{Myers}, P. C.},
 title = "{Protostar mass due to infall and dispersal}",
 journal = {\apj},
 archivePrefix = "arXiv",
 eprint = {0807.1270},
 keywords = {ISM: clouds, ISM: jets and outflows, stars: formation},
     year = 2008,
    month = nov,
   volume = 687,
    pages = {340-353},
      doi = {10.1086/591664},
   adsurl = {http://adsabs.harvard.edu/abs/2008ApJ...687..340M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{fedderrath2010,
 author = {{Federrath}, C. and {Banerjee}, R. and {Clark}, P. C. and {Klessen}, R. S.}, 
 title = "{Modeling collapse and accretion in turbulent gas clouds: Implementation and Comparison of sink particles in AMR and SPH}",
 journal = {\apj},
 archivePrefix = "arXiv",
 eprint = {1001.4456},
 keywords = {accretion, accretion disks, hydrodynamics, ISM: kinematics and dynamics, methods: numerical, shock waves, stars: formation},
     year = 2010,
    month = apr,
   volume = 713,
    pages = {269-290},
      doi = {10.1088/0004-637X/713/1/269},
   adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...713..269F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{truelove1997,
 author = {{Truelove}, J.K. and {Klein}, R. L. and {McKee}, C. F. and {Holliman}, J. H. and {Howell}, L. H. and {Greenough}, J. A. },
 title = "{The Jeans Condition: A new constraint on spatial resolution in simulations of isothermal self-gravitational hydrodynamics}",
 journal = {\apjl},
 keywords = {Gravitation, Hydrodynamics, ISM: clouds, Methods: numerical, stars: formation},
     year = 1997,
    month = nov,
   volume = 489,
      doi = {10.1086/310975},
   adsurl = {http://adsabs.harvard.edu/abs/1997ApJ...489L.179T},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{carroll2011,
 author = {{Carroll-Nellenback}, J. and {Shroyer}, B. and {Frank}, A. and {Ding}, Chen},
 title = "{Efficient parallelization for AMR MHD multiphysics calculations; Implementation in AstroBEAR}",
 journal = {ASP Conference Series},
 archivePrefix = "arXiv",
 eprint = {1110.1616},
     year = 2011,
    month = oct,
   adsurl = {http://adsabs.harvard.edu/abs/2011arXiv1110.1616C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{liu1996,
   author = {{Liu}, F. K.},
    title = "{Polytropic gas spheres: an approximate analytic solution of the Lane-Emden equation}",
  journal = {\mnras},
 keywords = {methods: analytical, stars: evolution, stars: neutron, white dwarfs, galaxy: kinematics and dynamics, galaxy: structure },
     year = 1996,
    month = aug,
   volume = 281,
    pages = {1197-1205},
 archivePrefix = "arXiv",
 eprint = {9512061},
   adsurl = {http://adsabs.harvard.edu/abs/1996MNRAS.281.1197L},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{falgout2002,
   author = {{Falgout}, R. and {Yang}, U.},
    title = "{hypre: a Library of High Performance Preconditioners}",
  journal = {\j-lect-notes-comp-sci},
     year = 2002,
   volume = 2331,
}

@ARTICLE{foster1993,
   author = {{Foster}, P.~N. and {Chevalier}, ~R. A.},
  journal = {\apj},
 keywords = {Stars: Pre-main-sequence, hydrodynamics, stars: formation},
     year = 1993,
    month = oct,
   volume = 416,
    pages = {303},
      doi = {10.1086/173236},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{hennebelle2003,
   author = {{Hennebelle}, A. P. and {Whitworth}, A. P. and {Gladwin}, P. P. and {Andre}, Ph.},
    title = "{Protostellar collapse induced by compression}",
  journal = {\mnras},
archivePrefix = "arXiv",
   eprint = {astro-ph/0206044},
 keywords = {gravitation, hydrodynamics, waves, stars: formation, ISM: clouds},
     year = 2003,
    month = apr,
   volume = 340,
    pages = {870-882},
      doi = {10.1046/j.1365-8711.2003.05584.x},
   adsurl = {http://adsabs.harvard.edu/abs/2003MNRAS.340..870H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}

}
@ARTICLE{bonnor1956,
   author = {{Bonnor}, W.B.},
    title = "{Boyle's law and gravitational instability}",
  journal = {\mnras},
     year = 1956,
    month = feb,
   volume = 116,
    pages = {351},
   adsurl = {http://adsabs.harvard.edu/abs/1956MNRAS.116..351B},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{ogino1999,
   author = {{Ogino}, S. and {Tomisaka}, K. and {Nakamura}, F.},
    title = "{Gravitational collapse of spherical interstellar clouds}",
  journal = {\pasj},
 keywords = {gravitation, hydrodynamics, interstellar: clouds, stars: formation},
     year = 1999,
    month = oct,
   volume = 51,
    pages = {637-651},
   adsurl = {http://adsabs.harvard.edu/abs/1999PASJ...51..637O},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@ARTICLE{ebert1955,
   author = {{Ebert}, R.},
  journal = {Z. Astrophys},
     year = 1955,
   volume = 37,
    pages = {217},
   adsurl = {http://adsabs.harvard.edu/abs/1955ZA.....37..217E},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{banerjee2004,
   author = {{Banerjee}, R. and {Pudritz}, R. E. and {Holmes}, L.},
    title = "{The formation and evolution of protostellar discs; three-dimensional adaptive mesh refinement hydrosimulations of collapsing, rotating Bonnor-Ebert spheres}",
  journal = {\mnras},
archivePrefix = "arXiv",
   eprint = {astro-ph/0408277},
 keywords = {accretion, accretion discs, hydrodynamics, methods: numerical, ISM: clouds, ISM: evolution},
     year = 2004,
    month = nov,
   volume = 355,
    pages = {248-272},
      doi = {10.1111/j.1365-2966.2004.08316.x},
   adsurl = {http://adsabs.harvard.edu/abs/2004MNRAS.355..248B},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@book{stahler2005,
author = {Stahler, S.W. and Palla, F.},
title = "{The Formation of Stars}",
year = {2005},
publisher = {Wiley-VCH},
pages = {242-245}
}

@book{spitzer1968,
author = {Spitzer, L.},
title = "{Nebulae and Interstellar Matter}",
year = {1968},
publisher = {The University of Chicago Press},
pages = 44
}

@book{difrancesco2007,
   author = {Di Francesco, J. and Evans, N. and Caselli, P. and Myers, P. and Shirley, Y. and Aikawa, Y. and Tafalla, M. },
    title = "{Protostars and Planets V}",
     year = {2007},
    publisher = {Tucson: Univ Arizona Press},
pages = 17
}
% editor = {{B.\~{}Reipurth, D.\~{}Jewitt, \& K.\~{}Keil}}

@book{ward-thompson2007,
   author = {Ward-Thompson, D. and Andre, D. and Crutcher, P. and Johnstone, D. and Onishi, T. and Wilson, C.},
    title = "{Protostars and Planets V}",
     year = {2007},
pages = 33,
    publisher = {Tucson: Univ Arizona Press}

}

% editor = {{B.\~{}Reipurth, D.\~{}Jewitt, \& K.\~{}Keil}}


@PHDTHESIS{andythesis2008,
   author = {{Cunningham}, A.~J.},
    title = "{Star formation driven mechanical feedback in molecular clouds}",
 keywords = {Magnetohydrodynamics, Star formation, Turbulence, Molecular clouds},
   school = {University of Rochester},
     year = 2008,
   adsurl = {http://adsabs.harvard.edu/abs/2008PhDT.........2C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@book{landau1968,
    author = {Landau, L. D. and Lifshitz, E. M.},
    citeulike-article-id = {7346990},
    citeulike-linkout-0 = {http://www.amazon.ca/exec/obidos/redirect?tag=citeulike09-20\&path=ASIN/B0019KDLHE},
    citeulike-linkout-1 = {http://www.amazon.de/exec/obidos/redirect?tag=citeulike01-21\&path=ASIN/B0019KDLHE},
    citeulike-linkout-2 = {http://www.amazon.fr/exec/obidos/redirect?tag=citeulike06-21\&path=ASIN/B0019KDLHE},
    citeulike-linkout-3 = {http://www.amazon.jp/exec/obidos/ASIN/B0019KDLHE},
    citeulike-linkout-4 = {http://www.amazon.co.uk/exec/obidos/ASIN/B0019KDLHE/citeulike00-21},
    citeulike-linkout-5 = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/B0019KDLHE},
    howpublished = {Hardcover},
    keywords = {1968},
    posted-at = {2010-06-21 17:22:45},
    priority = {2},
    publisher = {Addison-Wesley},
    title = {Fluid Mechanics},
    url = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/B0019KDLHE},
    year = {1968}
}


@book{leveque2002,
    author = {LeVeque, Randall J.},
    citeulike-article-id = {7346987},
    citeulike-linkout-0 = {http://www.amazon.ca/exec/obidos/redirect?tag=citeulike09-20\&path=ASIN/0521009243},
    citeulike-linkout-1 = {http://www.amazon.de/exec/obidos/redirect?tag=citeulike01-21\&path=ASIN/0521009243},
    citeulike-linkout-2 = {http://www.amazon.fr/exec/obidos/redirect?tag=citeulike06-21\&path=ASIN/0521009243},
    citeulike-linkout-3 = {http://www.amazon.jp/exec/obidos/ASIN/0521009243},
    citeulike-linkout-4 = {http://www.amazon.co.uk/exec/obidos/ASIN/0521009243/citeulike00-21},
    citeulike-linkout-5 = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/0521009243},
    citeulike-linkout-6 = {http://www.worldcat.org/isbn/0521009243},
    citeulike-linkout-7 = {http://books.google.com/books?vid=ISBN0521009243},
    citeulike-linkout-8 = {http://www.amazon.com/gp/search?keywords=0521009243\&index=books\&linkCode=qs},
    citeulike-linkout-9 = {http://www.librarything.com/isbn/0521009243},
    day = {26},
    edition = {1},
    howpublished = {Paperback},
    isbn = {0521009243},
    keywords = {2002},
    month = {August},
    posted-at = {2010-06-21 17:19:39},
    priority = {2},
    publisher = {Cambridge University Press},
    title = {Finite Volume Methods for Hyperbolic Problems (Cambridge Texts in Applied Mathematics)},
    url = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/0521009243},
    year = {2002}
}


@book{toro1999,
    author = {Toro, Eleuterio F.},
    citeulike-article-id = {7237678},
    citeulike-linkout-0 = {http://www.amazon.ca/exec/obidos/redirect?tag=citeulike09-20\&path=ASIN/3540252029},
    citeulike-linkout-1 = {http://www.amazon.de/exec/obidos/redirect?tag=citeulike01-21\&path=ASIN/3540252029},
    citeulike-linkout-10 = {http://www.worldcat.org/oclc/401321914},
    citeulike-linkout-2 = {http://www.amazon.fr/exec/obidos/redirect?tag=citeulike06-21\&path=ASIN/3540252029},
    citeulike-linkout-3 = {http://www.amazon.jp/exec/obidos/ASIN/3540252029},
    citeulike-linkout-4 = {http://www.amazon.co.uk/exec/obidos/ASIN/3540252029/citeulike00-21},
    citeulike-linkout-5 = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/3540252029},
    citeulike-linkout-6 = {http://www.worldcat.org/isbn/3540252029},
    citeulike-linkout-7 = {http://books.google.com/books?vid=ISBN3540252029},
    citeulike-linkout-8 = {http://www.amazon.com/gp/search?keywords=3540252029\&index=books\&linkCode=qs},
    citeulike-linkout-9 = {http://www.librarything.com/isbn/3540252029},
    day = {27},
    edition = {2nd},
    howpublished = {Softcover},
    isbn = {3540252029},
    keywords = {1999},
    month = {April},
    posted-at = {2010-06-21 16:59:09},
    priority = {2},
    publisher = {Springer},
    title = {Riemann Solvers and Numerical Methods for Fluid Dynamics: A Practical Introduction},
    url = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/3540252029},
    year = {1999}
}



@ARTICLE{berger1989,
   author = {{Berger}, M.~J. and {Colella}, P.},
    title = "{Local adaptive mesh refinement for shock hydrodynamics}",
  journal = {Journal of Computational Physics},
 keywords = {CONSERVATION LAWS, GRID GENERATION (MATHEMATICS), HYDRODYNAMICS, SHOCK WAVES, ALGORITHMS, BOUNDARY INTEGRAL METHOD, DISCONTINUITY, ERROR ANALYSIS, EULER EQUATIONS OF MOTION, NUMERICAL ANALYSIS},
     year = 1989,
    month = may,
   volume = 82,
    pages = {64-84},
      doi = {10.1016/0021-9991(89)90035-1},
   adsurl = {http://adsabs.harvard.edu/abs/1989JCoPh..82...64B},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{bachiller1996,
   author = {{Bachiller}, R.},
    title = "{Bipolar Molecular Outflows from Young Stars and Protostars}",
  journal = {\araa},
     year = 1996,
   volume = 34,
    pages = {111-154},
      doi = {10.1146/annurev.astro.34.1.111},
   adsurl = {http://adsabs.harvard.edu/abs/1996ARA%26A..34..111B},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{orlando2008,
   author = {{Orlando}, S. and {Bocchino}, F. and {Reale}, F. and {Peres}, G. and 
        {Pagano}, P.},
    title = "{The Importance of Magnetic-Field-Oriented Thermal Conduction in the Interaction of SNR Shocks with Interstellar Clouds}",
  journal = {\apj},
archivePrefix = "arXiv",
   eprint = {0801.1403},
 keywords = {Conduction, ISM: Clouds, ISM: Magnetic Fields, Magnetohydrodynamics: MHD, Shock Waves, ISM: Supernova Remnants},
     year = 2008,
    month = may,
   volume = 678,
    pages = {274-286},
      doi = {10.1086/529420},
   adsurl = {http://adsabs.harvard.edu/abs/2008ApJ...678..274O},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@ARTICLE{melioli2005,
   author = {{Melioli}, C. and {de Gouveia dal Pino}, E.~M. and {Raga}, A.
        },
    title = "{Multidimensional hydrodynamical simulations of radiative cooling SNRs-clouds interactions: an application to starburst environments}",
  journal = {\aap},
   eprint = {arXiv:astro-ph/0502104},
 keywords = {galaxies: starburst, hydrodynamics, shock waves, methods: N-body simulations, ISM: clouds, ISM: supernova remnants},
     year = 2005,
    month = nov,
   volume = 443,
    pages = {495-508},
      doi = {10.1051/0004-6361:20052679},
   adsurl = {http://adsabs.harvard.edu/abs/2005A%26A...443..495M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@ARTICLE{falgarone2004,
   author = {{Falgarone}, E. and {Hily-Blant}, P. and {Levrier}, F.},
    title = "{Structure of Molecular Clouds}",
  journal = {\apss},
 keywords = {molecular clouds, turbulence, fractals, intermittency, magnetic fields},
     year = 2004,
    month = aug,
   volume = 292,
    pages = {89-101},
      doi = {10.1023/B:ASTR.0000045004.70345.21},
   adsurl = {http://adsabs.harvard.edu/abs/2004Ap%26SS.292...89F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@ARTICLE{lauroesch2000,
   author = {{Lauroesch}, J.~T. and {Meyer}, D.~M. and {Blades}, J.~C.},
    title = "{Evidence of Interstellar NA I Structure at Scales Down to 15 AU in Low-Density Gas}",
  journal = {\apjl},
 keywords = {ISM: Clouds, ISM: Structure, Stars: Individual: Henry Draper Number: HD 32039, Stars: Individual: Henry Draper Number: HD 32040},
     year = 2000,
    month = nov,
   volume = 543,
    pages = {L43-L47},
      doi = {10.1086/318162},
   adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...543L..43L},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@article{diamond1989,
    abstract = {A three-station VLBI Galactic H I absorption experiment has been carriedout with baselines up to 600 km. The large collecting area of theEuropean VLBI Network consisting of the Lovell Telescope (Mark Ia), the100 m telescope at Effelsberg, and the Westerbork Synthesis RadioTelescope was necessary to achieve adequate sensitivity for these highangular resolution (0.05 arcsec) and high-velocity resolution (0.5 km/s)observations. The extragalactic sources 3C 138, 3C 147, and 3C 380 wereobserved. Changes in the local H I apparent absorption were observed inall three sources as a function of resolution. The changes are moststriking in the direction of 3C 138. The implied linear diameters are inthe range 25 AU with typical H I densities of 10,000-100,000/cu cm.},
    author = {Diamond, P. J. and Goss, W. M. and Romney, J. D. and Booth, R. S. and Kalberla, P. M. W. and Mebold, U.},
    citeulike-article-id = {7337980},
    citeulike-linkout-0 = {http://dx.doi.org/10.1086/168119},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1989ApJ...347..302D},
    doi = {10.1086/168119},
    journal = {\apj},
    keywords = {1989},
    month = {December},
    pages = {302--306},
    posted-at = {2010-06-17 18:56:35},
    priority = {2},
    title = {The structure of the interstellar medium at the 25 AU scale},
    url = {http://dx.doi.org/10.1086/168119},
    volume = {347},
    year = {1989}
}


@ARTICLE{gardiner2001,
   author = {{Gardiner}, T.~A. and {Frank}, A.},
    title = "{Magnetic Collimation in Planetary Nebulae}",
  journal = {\apj},
 keywords = {ISM: Jets and Outflows, ISM: Magnetic Fields, Magnetic Fields, Magnetohydrodynamics: MHD, ISM: Planetary Nebulae: General},
     year = 2001,
    month = aug,
   volume = 557,
    pages = {250-255},
      doi = {10.1086/321494},
   adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...557..250G},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{gardiner2000,
   author = {{Gardiner}, T.~A. and {Frank}, A. and {Jones}, T.~W. and {Ryu}, D.
        },
    title = "{Influence of Magnetic Fields on Pulsed, Radiative Jets}",
  journal = {\apj},
 keywords = {HYDRODYNAMICS, ISM: JETS AND OUTFLOWS, MAGNETOHYDRODYNAMICS: MHD, SHOCK WAVES, STARS: MAGNETIC FIELDS, STARS: PRE-MAIN-SEQUENCE},
     year = 2000,
    month = feb,
   volume = 530,
    pages = {834-850},
      doi = {10.1086/308391},
   adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...530..834G},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{frank1996kh,
   author = {{Frank}, A. and {Jones}, T.~W. and {Ryu}, D. and {Gaalaas}, J.~B.
        },
    title = "{The Magnetohydrodynamic Kelvin-Helmholtz Instability: A Two-dimensional Numerical Study}",
  journal = {\apj},
   eprint = {arXiv:astro-ph/9510115},
 keywords = {INSTABILITIES, METHODS: NUMERICAL, MAGNETOHYDRODYNAMICS: MHD, TURBULENCE},
     year = 1996,
    month = apr,
   volume = 460,
    pages = {777-+},
      doi = {10.1086/177009},
   adsurl = {http://adsabs.harvard.edu/abs/1996ApJ...460..777F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{frank1998,
   author = {{Frank}, A. and {Ryu}, D. and {Jones}, T.~W. and {Noriega-Crespo}, A.
        },
    title = "{Effects of Cooling on the Propagation of Magnetized Jets}",
  journal = {\apjl},
   eprint = {arXiv:astro-ph/9711250},
 keywords = {STARS: FORMATION, ISM: JETS AND OUTFLOWS, MAGNETOHYDRODYNAMICS: MHD},
     year = 1998,
    month = feb,
   volume = 494,
    pages = {L79+},
      doi = {10.1086/311159},
   adsurl = {http://adsabs.harvard.edu/abs/1998ApJ...494L..79F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{elmegreen2004,
   author = {{Elmegreen}, B.~G. and {Scalo}, J.},
    title = "{Interstellar Turbulence I: Observations and Processes}",
  journal = {\araa},
   eprint = {arXiv:astro-ph/0404451},
     year = 2004,
    month = sep,
   volume = 42,
    pages = {211-273},
      doi = {10.1146/annurev.astro.41.011802.094859},
   adsurl = {http://adsabs.harvard.edu/abs/2004ARA%26A..42..211E},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{hatchell2005,
   author = {{Hatchell}, J. and {Richer}, J.~S. and {Fuller}, G.~A. and {Qualtrough}, C.~J. and 
        {Ladd}, E.~F. and {Chandler}, C.~J.},
    title = "{Star formation in Perseus. Clusters, filaments and the conditions for star formation}",
  journal = {\aap},
 keywords = {stars: formation, submillimeter, dust, extinction, ISM: molecules, ISM: clouds, ISM: structure},
     year = 2005,
    month = sep,
   volume = 440,
    pages = {151-161},
      doi = {10.1051/0004-6361:20041836},
   adsurl = {http://adsabs.harvard.edu/abs/2005A%26A...440..151H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{vannier2001,
   author = {{Vannier}, L. and {Lemaire}, J.~L. and {Field}, D. and {Pineau des For{\^e}ts}, G. and 
        {Pijpers}, F.~P. and {Rouan}, D.},
    title = "{H_{2} infrared emission and the formation of dense structures in the Orion molecular cloud}",
  journal = {\aap},
 keywords = {ISM: Individual Objects: OMC1, ISM: Kinematics and Dynamics, ISM: Molecules, Shock Waves, Infrared: ISM: Lines and Bands},
     year = 2001,
    month = feb,
   volume = 366,
    pages = {651-661},
      doi = {10.1051/0004-6361:20000258},
   adsurl = {http://adsabs.harvard.edu/abs/2001A%26A...366..651V},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{raga1987,
   author = {{Raga}, A.~C. and {Bohm}, K.~H.},
    title = "{Time-dependent bow shocks and the condensation structure of Herbig-Haro objects}",
  journal = {\apj},
 keywords = {BOW WAVES, CONDENSING, HERBIG-HARO OBJECTS, SHOCK WAVES, STELLAR MODELS, STELLAR STRUCTURE, H ALPHA LINE, PRE-MAIN SEQUENCE STARS, STELLAR EVOLUTION, THERMAL INSTABILITY, TIME DEPENDENCE},
     year = 1987,
    month = dec,
   volume = 323,
    pages = {193-210},
      doi = {10.1086/165819},
   adsurl = {http://adsabs.harvard.edu/abs/1987ApJ...323..193R},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{hennebelle2006,
   author = {{Hennebelle}, P. and {Passot}, T.},
    title = "{Influence of Alfv{\'e}n waves on thermal instability in the interstellar medium}",
  journal = {\aap},
   eprint = {arXiv:astro-ph/0510425},
 keywords = {ISM: instabilities, magnetohydrodynamics, turbulence, ISM: clouds, ISM: magnetic fields},
     year = 2006,
    month = mar,
   volume = 448,
    pages = {1083-1093},
      doi = {10.1051/0004-6361:20053510},
   adsurl = {http://adsabs.harvard.edu/abs/2006A%26A...448.1083H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{faison2001,
   author = {{Faison}, M.~D. and {Goss}, W.~M.},
    title = "{The Structure of the Cold Neutral Interstellar Medium on 10-100 AU Scales}",
  journal = {\aj},
   eprint = {arXiv:astro-ph/0011460},
 keywords = {ISM: H I, ISM: Structure, Techniques: Interferometric},
     year = 2001,
    month = may,
   volume = 121,
    pages = {2706-2722},
      doi = {10.1086/320369},
   adsurl = {http://adsabs.harvard.edu/abs/2001AJ....121.2706F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{deshpande2000,
   author = {{Deshpande}, A.~A.},
    title = "{The small-scale structure in interstellar Hi: a resolvable puzzle}",
  journal = {\mnras},
   eprint = {arXiv:astro-ph/0005336},
 keywords = {PULSARS: GENERAL, ISM: CLOUDS, ISM: MOLECULES, ISM: STRUCTURE, RADIO LINES: ISM},
     year = 2000,
    month = sep,
   volume = 317,
    pages = {199-204},
      doi = {10.1046/j.1365-8711.2000.03631.x},
   adsurl = {http://adsabs.harvard.edu/abs/2000MNRAS.317..199D},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{heiles1997,
   author = {{Heiles}, C.},
    title = "{Tiny-Scale Atomic Structure and the Cold Neutral Medium}",
  journal = {\apj},
 keywords = {ISM: CLOUDS, ISM: STRUCTURE, TURBULENCE},
     year = 1997,
    month = may,
   volume = 481,
    pages = {193-+},
      doi = {10.1086/304033},
   adsurl = {http://adsabs.harvard.edu/abs/1997ApJ...481..193H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{rosen2004,
    abstract = {We present three-dimensional hydrodynamic simulations of jets as a modelfor protostellar outflows. We investigate molecular jets which areinitially heavier, equal or lighter than a uniform ambient molecularmedium, as well as a ballistic atomic jet, with the aim ofdistinguishing the resulting structures and relating them to variousproposed protostellar evolutionary stages. We modify the ZEUS numericalcode, to include time-dependent molecular hydrogen chemistry, a limitedequilibrium C and O chemistry, and a detailed cooling function. We findhighly focussed and accelerated flow patterns for outflows driven bymolecular jets, caused by the combined strong cooling, small imposed jetshear and precession. We also find shoulders in the interface withassociated shocks visible in our simulated near-infrared H\_2 images. Theshoulder location relative to the front of the bow shock distinguishesthe relative density. Apart from this, the outflow structures are quitesimilar provided the jet is molecular. The ratio of jet power to H\_2 1-0S(1) line luminosity (increasingly required to interpret observations),is generally in the range 80-600. Sub-millimetre CO properties,including a velocity-position and velocity-channel diagram; arepresented. We compare mass-velocity relationships derived directly andvia the simulated CO data: significant systematic differences areuncovered. For the future, we identify fine-scale structure in therotational CO 2-1 and CO 14-13 rotational lines which can be resolvedwith the millimetre array ALMA and the Herschel (FIRST) Observatory. Weidentify highly collimated outflows in the near-infrared that can beinterpreted by this model.},
    author = {Rosen, A. and Smith, M. D.},
    citeulike-article-id = {7337938},
    citeulike-linkout-0 = {http://dx.doi.org/10.1051/0004-6361:20031566},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2004A\&A...413..593R},
    doi = {10.1051/0004-6361:20031566},
    journal = {\aap},
    keywords = {2004},
    month = {January},
    pages = {593--607},
    posted-at = {2010-06-17 18:29:13},
    priority = {2},
    title = {Numerical simulations of highly collimated protostellar outflows. The effects of relative density},
    url = {http://dx.doi.org/10.1051/0004-6361:20031566},
    volume = {413},
    year = {2004}
}


@article{saxton2005,
    abstract = {We present two-dimensional slab-jet simulations of jets in inhomogeneousmedia consisting of a tenuous hot medium populated with a small fillingfactor by warm, dense clouds. The simulations are relevant to thestructure and dynamics of sources such as gigahertz peak spectrum andcompact steep spectrum (CSS) radio galaxies, high-redshift radiogalaxies and radio galaxies in cooling flows. The jets are disrupted toa degree depending upon the filling factor of the clouds. With a smallfilling factor, the jet retains some forward momentum but also forms ahalo or bubble around the source. At larger filling factors channels areformed in the cloud distribution through which the jet plasma flows anda hierarchical structure consisting of nested lobes and an outerenclosing bubble results. We suggest that the CSS quasar 3C 48 is anexample of a low filling factor jet-interstellar medium interactionwhile M87 may be an example of the higher filling factor type ofinteraction. Jet disruption occurs primarily as a result ofKelvin-Helmholtz instabilities driven by turbulence in the radio cocoonnot through direct jet-cloud interactions, although there are someexamples of these. In all radio galaxies whose morphology may be theresult of jet interactions with an inhomogeneous interstellar medium weexpect that the dense clouds will be optically observable as a result ofradiative shocks driven by the pressure of the radio cocoon. We alsoexpect that the radio galaxies will possess faint haloes ofradio-emitting material well beyond the observable jet structure.},
    archivePrefix = {arXiv},
    author = {Saxton, C. J. and Bicknell, G. V. and Sutherland, R. S. and Midgley, S.},
    citeulike-article-id = {174260},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0502367},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0502367},
    citeulike-linkout-2 = {http://dx.doi.org/10.1111/j.1365-2966.2005.08962.x},
    citeulike-linkout-3 = {http://www.ingentaconnect.com/content/bsc/mnr/2005/00000359/00000002/art00040},
    citeulike-linkout-4 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2005MNRAS.359..781S},
    doi = {10.1111/j.1365-2966.2005.08962.x},
    eprint = {astro-ph/0502367},
    issn = {0035-8711},
    journal = {\mnras},
    keywords = {2005},
    month = {May},
    number = {2},
    pages = {781--800},
    posted-at = {2010-06-17 18:18:57},
    priority = {2},
    publisher = {Blackwell Publishing},
    title = {Interactions of jets with inhomogeneous cloudy media},
    url = {http://dx.doi.org/10.1111/j.1365-2966.2005.08962.x},
    volume = {359},
    year = {2005}
}


@article{osullivan2002,
    abstract = {We present simulations of the propagation of non-adiabatic molecularjets into an inhomogeneous ambient medium. The jets have inflowconditions described by a MHD jet model where the shape of the magneticfield lines is prescribed near the source. Ambient density profiles arechosen to represent the transition zone between the outer regions of amolecular cloud and the ISM. We have scaled the atomic and molecularcooling rates to appropriate levels in order to properly resolve alllength scales involved. With the inclusion of source variability, thesimulations reproduce several observational features of molecular jetssuch as molecular cavities. Additionally, we find similarities betweentheory and observation for the ionization fraction along the jet. Thelateral extent of the internal working surfaces is found to be sensitiveto the environment. We also present preliminary results from a method ofcalculating emission line maps using only fundamental state variablesthat seems to reproduce the observed filamentary Balmer emission onshock fronts.},
    author = {O'Sullivan, S. and Lery, T.},
    booktitle = {Revista Mexicana de Astronomia y Astrofisica Conference Series},
    citeulike-article-id = {7337915},
    citeulike-linkout-0 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2002RMxAC..13...98O},
    editor = {{W.\~{}J.\~{}Henney, W.\~{}Steffen, L.\~{}Binette, \& A.\~{}Raga}},
    journal = {Revista Mexicana de Astronomia y Astrofisica},
    keywords = {2002},
    month = {June},
    pages = {98--102},
    posted-at = {2010-06-17 18:12:46},
    priority = {2},
    series = {Revista Mexicana de Astronomia y Astrofisica Conference Series},
    title = {MHD Jets in Inhomogeneous Media},
    url = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2002RMxAC..13...98O},
    volume = {13},
    year = {2002}
}

@article{yirak2009,
   author = {{Yirak}, K. and {Frank}, A. and {Cunningham}, A.~J. and {Mitran}, S.},
    title = "{Hypersonic Buckshot: Astrophysical Jets as Heterogeneous Collimated Plasmoids}",
  journal = {\apj},
archivePrefix = "arXiv",
   eprint = {0806.0038},
 keywords = {hydrodynamics, ISM: Herbig-Haro objects, ISM: jets and outflows},
     year = 2009,
    month = apr,
   volume = 695,
    pages = {999-1005},
      doi = {10.1088/0004-637X/695/2/999},
   adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...695..999Y},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{niklaus2009,
   author = {{Niklaus}, M. and {Schmidt}, W. and {Niemeyer}, J.~C.},
    title = "{Two-dimensional adaptive mesh refinement simulations of colliding flows}",
  journal = {\aap},
archivePrefix = "arXiv",
   eprint = {0907.1239},
 keywords = {hydrodynamics, turbulence, instabilities, ISM: kinematics and dynamics, methods: numerical, ISM: clouds},
     year = 2009,
    month = nov,
   volume = 506,
    pages = {1065-1070},
      doi = {10.1051/0004-6361/200912483},
   adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...506.1065N},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@article{andy2009b,
   author = {{Cunningham}, A.~J. and {Frank}, A. and {Carroll}, J. and {Blackman}, E.~G. and 
        {Quillen}, A.~C.},
    title = "{Protostellar Outflow Evolution in Turbulent Environments}",
  journal = {\apj},
archivePrefix = "arXiv",
   eprint = {0804.4197},
 keywords = {hydrodynamics, ISM: clouds, ISM: jets and outflows, stars: formation, turbulence},
     year = 2009,
    month = feb,
   volume = 692,
    pages = {816-826},
      doi = {10.1088/0004-637X/692/1/816},
   adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...692..816C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@article{vanloo2007,
    abstract = {Aims.Our aim is to understand the formation of a magnetically dominatedmolecular cloud out of an atomic cloud.  Methods: A thermally stablewarm atomic cloud is initially in static equilibrium with thesurrounding hot ionised gas. A shock propagating through the hot mediuminteracts with the cloud. We follow the dynamical evolution of the cloudwith a time-dependent axisymmetric magnetohydrodynamic code.  Results:As a fast-mode shock propagates through the cloud, the gas behind itbecomes thermally unstable. The beta value of the gas also becomesmuch smaller than the initial value of order unity. These conditions areideal for magnetohydrodynamic waves to produce high-density clumpsembedded in a rarefied warm medium. A slow-mode shock follows thefast-mode shock. Behind this shock a dense shell forms, whichsubsequently fragments. This is a primary region for the formation ofmassive stars. Our simulations show that only weak and moderate-strengthshocks can form cold clouds which have properties typical of giantmolecular clouds.},
    archivePrefix = {arXiv},
    author = {van Loo, S. and Falle, S. A. E. G. and Hartquist, T. W. and Moore, T. J. T.},
    citeulike-article-id = {5800853},
    citeulike-linkout-0 = {http://arxiv.org/abs/0706.0434},
    citeulike-linkout-1 = {http://arxiv.org/pdf/0706.0434},
    citeulike-linkout-2 = {http://dx.doi.org/10.1051/0004-6361:20077430},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2007A\&A...471..213V},
    doi = {10.1051/0004-6361:20077430},
    eprint = {0706.0434},
    journal = {\aap},
    keywords = {2007, clumps},
    month = {August},
    pages = {213--218},
    posted-at = {2009-09-18 01:51:44},
    priority = {2},
    title = {Shock-triggered formation of magnetically-dominated clouds},
    url = {http://dx.doi.org/10.1051/0004-6361:20077430},
    volume = {471},
    year = {2007}
}


@article{carver2009,
        abstract = {},
        author = {Carver, R. and Frank, A. and Hartigan, P. and Cunningham, A.J. and Palmer, J. and Yirak, K.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
        priority = {},
        title = {},
        url = {},
        volume = {},
        year = {in prep.}
}

@article{preibisch2002,
    abstract = {We investigate the stellar population and star formation history of theUpper Scorpius OB association, the most nearby region of recent massivestar formation, over the full stellar mass range from 0.1 to 20M<SUB>solar</SUB>. The first part of this paper describes an extensionof our large spectroscopic survey (Preibisch et al., published in 2001)for low-mass pre-main-sequence (PMS) stars in Upper Scorpius. Using themultiobject spectrograph 2dF at the Anglo-Australian Telescope, weobtained spectra of 469 stars with magnitudes R=12.5-18.0 in a 6deg<SUP>2</SUP> area. Among these, we find 68 new PMS stars, nearly allof them M-type stars, by their strong lithium absorption lines. Thetotal area covered by our 2dF survey is now 9 deg<SUP>2</SUP> andcontains 166 new PMS stars. Combining these results with our earlierinvestigation (Preibisch \& Zinnecker) yields a sample of 250 PMSstars in the mass range \~{}0.1 to \~{}2 M<SUB>solar</SUB>. The location ofthese stars in the HR diagram suggests a mean age of 5 Myr without asignificant age spread. In the second part of this paper, we alsoconsider the population of 114 high-mass members identified in detailedHipparcos studies. We construct a combined HR diagram for the 364 high-and low-mass members and find that the whole stellar population is verywell characterized by a very narrow age distribution around 5 Myr. Weestimate individual masses for all members and construct an empiricalmass function covering the mass range from 0.1 up to 20M<SUB>solar</SUB>. A power-law fit to the mass function gives a slope ofalpha\~{}-2.6 above \~{}2 M<SUB>solar</SUB> and a much flatter slope(alpha\~{}-0.9) below \~{}0.6 M<SUB>solar</SUB>. The initial mass functionof Upper Sco is not identical, but within the errors consistent withrecent determinations of the field initial mass function. There iscertainly no deficit of low-mass stars in the Upper Sco OB association,but rather a small excess of low-mass stars. Our results on the stellarage distribution confirm earlier indications that the star formationprocess in Upper Sco was triggered and support previous conjectures thatthe triggering event was a supernova shock wave originating from thenearby Upper Centaurus-Lupus association.},
    author = {Preibisch, T. and Brown, A. G. A. and Bridges, T. and Guenther, E. and Zinnecker, H.},
    citeulike-article-id = {5800777},
    citeulike-linkout-0 = {http://dx.doi.org/10.1086/341174},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2002AJ....124..404P},
    doi = {10.1086/341174},
    journal = {\aj},
    keywords = {2002, molecular-clouds},
    month = {July},
    pages = {404--416},
    posted-at = {2009-09-18 00:10:48},
    priority = {2},
    title = {Exploring the Full Stellar Population of the Upper Scorpius OB Association},
    url = {http://dx.doi.org/10.1086/341174},
    volume = {124},
    year = {2002}
}


@article{zeldovich2002,
        abstract = {},
        author = {Zel'dovich, Ya. B. and Raizer, Yu. P.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {Physics of Shock Waves and High-Temperature Hydrodynamic Phenomena (Dover)},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
        priority = {},
        title = {},
        url = {},
        volume = {},
        year = {2002}
}

@article{choudhuri1998,
        abstract = {},
        author = {Choudhuri, A.R.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {The Physics of Fluids and Plasmas (Cambridge University Press)},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
        priority = {},
        title = {},
        url = {},
        volume = {},
        year = {1998}
}

@article{hirschel2005,
        abstract = {},
        author = {Hirschel, E.H.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {Basics of Aerothermodynamics (Berlin: Springer)},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
        priority = {},
        title = {},
        url = {},
        volume = {},
        year = {2005}
}


@article{dysonwilliams1997,
        abstract = {},
        author = {Dyson, J.E. and Williams, D.A.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {The Physics of the Interstellar Medium, 2nd Ed. (Taylor \& Francis)},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
        priority = {},
        title = {},
        url = {},
        volume = {},
        year = {1997}
}


@article{chandrasekhar1961,
        abstract = {},
        author = {Chandrasekhar, S.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {Hydrodynamic and Hydromagnetic Stability (New York: Dover)},
        keywords = {},
        month = {},
        pages = {},
        posted-at = {},
        priority = {},
        title = {},
        url = {},
        volume = {},
        year = {1961}
}


@ARTICLE{springel2005,
   author = {{Springel}, V.},
    title = "{The cosmological simulation code GADGET-2}",
  journal = {\mnras},
   eprint = {arXiv:astro-ph/0505010},
 keywords = {methods: numerical, galaxies: interactions, dark matter},
     year = 2005,
    month = dec,
   volume = 364,
    pages = {1105-1134},
      doi = {10.1111/j.1365-2966.2005.09655.x},
   adsurl = {http://adsabs.harvard.edu/abs/2005MNRAS.364.1105S},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@book{aarseth2009nbody,
    author = {Aarseth, Sverre J.},
    citeulike-article-id = {7347576},
    citeulike-linkout-0 = {http://www.amazon.ca/exec/obidos/redirect?tag=citeulike09-20\&amp;path=ASIN/0521121531},
    citeulike-linkout-1 = {http://www.amazon.de/exec/obidos/redirect?tag=citeulike01-21\&amp;path=ASIN/0521121531},
    citeulike-linkout-2 = {http://www.amazon.fr/exec/obidos/redirect?tag=citeulike06-21\&amp;path=ASIN/0521121531},
    citeulike-linkout-3 = {http://www.amazon.jp/exec/obidos/ASIN/0521121531},
    citeulike-linkout-4 = {http://www.amazon.co.uk/exec/obidos/ASIN/0521121531/citeulike00-21},
    citeulike-linkout-5 = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/0521121531},
    citeulike-linkout-6 = {http://www.worldcat.org/isbn/0521121531},
    citeulike-linkout-7 = {http://books.google.com/books?vid=ISBN0521121531},
    citeulike-linkout-8 = {http://www.amazon.com/gp/search?keywords=0521121531\&index=books\&linkCode=qs},
    citeulike-linkout-9 = {http://www.librarything.com/isbn/0521121531},
    day = {15},
    edition = {1},
    howpublished = {Paperback},
    isbn = {0521121531},
    keywords = {2009},
    month = {October},
    posted-at = {2010-06-22 01:22:11},
    priority = {2},
    publisher = {Cambridge University Press},
    title = {Gravitational N-Body Simulations: Tools and Algorithms (Cambridge Monographs on Mathematical Physics)},
    url = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/0521121531},
    year = {2009}
}


@book{grigoryev2002pic,
    abstract = {{Algorithms known as ``particle'' methods, whose characteristic feature is the discretization technique when the set of discrete objects is introduced, which are model ``particles'' considered as some mesh of moving nodes, are becoming more and more widespread in mathematical modelling. Until recently, particle methods have mainly been developed as an alternative to classical numerical methods for solving problems in plasma physics. As a result, no specialized monographs on this subject had been available. The aim of this book is to fill the gap in literature on this subject and deals with combined Lagrangian-Eulerian schemes of the ``particle-in-cell'' type, the most widespread among particle methods. The authors describe a universal approach to the construction of such algorithms.   <P>The approach is based on splitting the initial problem by which the auxiliary problem with a hyperbolic (divergent) operator is separated. After special discretization of the solution, such a splitting naturally leads to the well-known schemes of ``particle-in-cell'' methods. Examples of calculations in this book give the reader an idea of the capabilities of particle-in-cell methods, their requirements to computers, and the degree of precision that can be achieved. This book is primarily intended for specialists in calculations, who want to get a general idea of numerical particle-in-cell methods and the sphere of their applications. As a methodological guide, it will be of interest to undergraduate and postgraduate students, mathematicians and physicists specializing in mathematical modelling.}},
    author = {Grigoryev, Yu. N. and Vshivkov, V. A. and Fedoruk, M. P.},
    citeulike-article-id = {2709656},
    citeulike-linkout-0 = {http://www.amazon.ca/exec/obidos/redirect?tag=citeulike09-20\&amp;path=ASIN/9067643688},
    citeulike-linkout-1 = {http://www.amazon.de/exec/obidos/redirect?tag=citeulike01-21\&amp;path=ASIN/9067643688},
    citeulike-linkout-2 = {http://www.amazon.fr/exec/obidos/redirect?tag=citeulike06-21\&amp;path=ASIN/9067643688},
    citeulike-linkout-3 = {http://www.amazon.jp/exec/obidos/ASIN/9067643688},
    citeulike-linkout-4 = {http://www.amazon.co.uk/exec/obidos/ASIN/9067643688/citeulike00-21},
    citeulike-linkout-5 = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/9067643688},
    citeulike-linkout-6 = {http://www.worldcat.org/isbn/9067643688},
    citeulike-linkout-7 = {http://books.google.com/books?vid=ISBN9067643688},
    citeulike-linkout-8 = {http://www.amazon.com/gp/search?keywords=9067643688\&index=books\&linkCode=qs},
    citeulike-linkout-9 = {http://www.librarything.com/isbn/9067643688},
    day = {31},
    howpublished = {Hardcover},
    isbn = {9067643688},
    keywords = {2002},
    month = {July},
    posted-at = {2010-06-22 01:16:31},
    priority = {2},
    publisher = {Walter de Gruyter Inc},
    title = {Numerical ``Particle-In-Cell'' Methods: Theory and Applications},
    url = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/9067643688},
    year = {2002}
}


@book{liu2003sph,
    author = {Liu, G. R. and Liu, M. B.},
    citeulike-article-id = {7347572},
    citeulike-linkout-0 = {http://www.amazon.ca/exec/obidos/redirect?tag=citeulike09-20\&amp;path=ASIN/9812384561},
    citeulike-linkout-1 = {http://www.amazon.de/exec/obidos/redirect?tag=citeulike01-21\&amp;path=ASIN/9812384561},
    citeulike-linkout-2 = {http://www.amazon.fr/exec/obidos/redirect?tag=citeulike06-21\&amp;path=ASIN/9812384561},
    citeulike-linkout-3 = {http://www.amazon.jp/exec/obidos/ASIN/9812384561},
    citeulike-linkout-4 = {http://www.amazon.co.uk/exec/obidos/ASIN/9812384561/citeulike00-21},
    citeulike-linkout-5 = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/9812384561},
    citeulike-linkout-6 = {http://www.worldcat.org/isbn/9812384561},
    citeulike-linkout-7 = {http://books.google.com/books?vid=ISBN9812384561},
    citeulike-linkout-8 = {http://www.amazon.com/gp/search?keywords=9812384561\&index=books\&linkCode=qs},
    citeulike-linkout-9 = {http://www.librarything.com/isbn/9812384561},
    howpublished = {Hardcover},
    isbn = {9812384561},
    keywords = {2003},
    posted-at = {2010-06-22 01:14:11},
    priority = {2},
    publisher = {World Scientific Publishing Company},
    title = {Smoothed Particle Hydrodynamics: A Meshfree Particle Method},
    url = {http://www.amazon.com/exec/obidos/redirect?tag=citeulike07-20\&path=ASIN/9812384561},
    year = {2003}
}


@ARTICLE{monaghan1992sph,
   author = {{Monaghan}, J.~J.},
    title = "{Smoothed particle hydrodynamics}",
  journal = {\araa},
 keywords = {COMPUTATIONAL FLUID DYNAMICS, FINITE DIFFERENCE THEORY, HYDRODYNAMICS, KERNEL FUNCTIONS, PARTICLE ENERGY, PARTICLE MASS, ANGULAR MOMENTUM, PARTIAL DIFFERENTIAL EQUATIONS, PARTICLE IN CELL TECHNIQUE, PRESSURE GRADIENTS},
     year = 1992,
   volume = 30,
    pages = {543-574},
      doi = {10.1146/annurev.aa.30.090192.002551},
   adsurl = {http://adsabs.harvard.edu/abs/1992ARA%26A..30..543M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@article{agertz2007,
    abstract = {We have carried out a comparison study of hydrodynamical codes byinvestigating their performance in modelling interacting multiphasefluids. The two commonly used techniques of grid and smoothed particlehydrodynamics (SPH) show striking differences in their ability to modelprocesses that are fundamentally important across many areas ofastrophysics. Whilst Eulerian grid based methods are able to resolve andtreat important dynamical instabilities, such as Kelvin-Helmholtz orRayleigh-Taylor, these processes are poorly or not at all resolved byexisting SPH techniques. We show that the reason for this is that SPH,at least in its standard implementation, introduces spurious pressureforces on particles in regions where there are steep density gradients.This results in a boundary gap of the size of an SPH smoothing kernelradius over which interactions are severely damped.},
    archivePrefix = {arXiv},
    author = {Agertz, O. and Moore, B. and Stadel, J. and Potter, D. and Miniati, F. and Read, J. and Mayer, L. and Gawryszczak, A. and Kravtsov, A. and {AA. Nordlund} and Pearce, F. and Quilis, V. and Rudd, D. and Springel, V. and Stone, J. and Tasker, E. and Teyssier, R. and Wadsley, J. and Walder, R.},
    citeulike-article-id = {1673919},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0610051},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0610051},
    citeulike-linkout-2 = {http://www.blackwell-synergy.com/doi/abs/10.1111/j.1365-2966.2007.12183.x},
    citeulike-linkout-3 = {http://dx.doi.org/10.1111/j.1365-2966.2007.12183.x},
    citeulike-linkout-4 = {http://www.ingentaconnect.com/content/bsc/mnr/2007/00000380/00000003/art00008},
    citeulike-linkout-5 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2007MNRAS.380..963A},
    doi = {10.1111/j.1365-2966.2007.12183.x},
    eprint = {astro-ph/0610051},
    issn = {0035-8711},
    journal = {\mnras},
    keywords = {2007, clumps},
    month = {September},
    number = {3},
    pages = {963--978},
    posted-at = {2009-09-17 23:42:37},
    priority = {2},
    publisher = {Blackwell Publishing},
    title = {Fundamental differences between SPH and grid methods},
    url = {http://dx.doi.org/10.1111/j.1365-2966.2007.12183.x},
    volume = {380},
    year = {2007}
}



@article{patnaude2005,
    abstract = {We present optical observations and two-dimensional hydrodynamicmodeling of an isolated shocked ISM cloud. Halpha images taken in1992.6 and 2003.7 of a small optical emission cloud along thesouthwestern limb of the Cygnus Loop were used to measure positionaldisplacements of \~{}0.1" yr<SUP>-1</SUP> for surrounding Balmer-dominatedemission filaments and 0.025"-0.055" yr<SUP>-1</SUP> for internal cloudemission features. These measurements imply transverse velocities of\~{}=250 and \~{}=80-140 km s<SUP>-1</SUP> for ambient ISM and internal cloudshocks, respectively. A lack of observed turbulent gas stripping at thecloud-ISM boundary in the Halpha images suggests that there is not anabrupt density change at the cloud-ISM boundary. Also, the complex shockstructure visible within the cloud indicates that the cloud's internaldensity distribution is two-phased-a smoothly varying background densitythat is populated by higher density clumps. Guided by the Halphaimages, we present model results for a shock interacting with anonuniform ISM cloud. We find that this cloud can be well modeled by asmoothly varying power-law core with a density contrast of \~{}4 times theambient density, surrounded by a low-density envelope with a Lorentzianprofile. The lack of sharp density gradients in such a model inhibitsthe growth of Kelvin-Helmholtz instabilities, consistent with thecloud's appearance. Our model results also suggest that cloud clumpshave densities \~{}10 times the ambient ISM density and account for \~{}30\% ofthe total cloud volume. Moreover, the observed spacing of internal cloudshocks and model simulations indicate that the distance between clumpsis \~{}4 clump radii. We conclude that this diffuse ISM cloud is bestmodeled by a smoothly varying, low-density distribution coupled tohigher density, moderately spaced internal clumps.},
    archivePrefix = {arXiv},
    author = {Patnaude, D. J. and Fesen, R. A.},
    citeulike-article-id = {5800751},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0507330},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0507330},
    citeulike-linkout-2 = {http://dx.doi.org/10.1086/452627},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2005ApJ...633..240P},
    doi = {10.1086/452627},
    eprint = {astro-ph/0507330},
    journal = {\apj},
    keywords = {2005, clumps},
    month = {November},
    pages = {240--247},
    posted-at = {2009-09-17 23:40:52},
    priority = {2},
    title = {Model Simulations of a Shock-Cloud Interaction in the Cygnus Loop},
    url = {http://dx.doi.org/10.1086/452627},
    volume = {633},
    year = {2005}
}



@article{steffen2004,
    abstract = {Hydrodynamical, axisymmetric simulations and analytic calculations arepresented for the interaction of a fast tenuous stellar wind with aspherical distribution of high-density clouds or clumps embedded in astationary intercloud medium with an approximately inverse squaredensity fall-off. Two distinct cases are studied. In the first case,clumps are formed by dynamic and thermal instabilities in the shockedwind. In the second case clumps, are assumed to have been formed byinhomogeneities in the AGB wind, prior to the onset of the fast wind. Wefind that the velocity distribution of these two cases is verydifferent. However, in both cases the ensemble of clumps develops apositive velocity gradient with distance, and the kinematics mightprovide information on the evolutionary stage of the nebula.},
    author = {Steffen, W. and L\'{o}pez, J. A.},
    citeulike-article-id = {5800746},
    citeulike-linkout-0 = {http://dx.doi.org/10.1086/422445},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2004ApJ...612..319S},
    doi = {10.1086/422445},
    journal = {\apj},
    keywords = {1995, clumps, pne},
    month = {September},
    pages = {319--331},
    posted-at = {2009-09-17 23:35:04},
    priority = {2},
    title = {On the Velocity Structure in Clumpy Planetary Nebulae},
    url = {http://dx.doi.org/10.1086/422445},
    volume = {612},
    year = {2004}
}


@article{andy2009,
    abstract = {A description is given of the algorithms implemented in the AstroBEARadaptive mesh-refinement code for ideal magnetohydrodynamics. The codeprovides several high-resolution shock-capturing schemes which areconstructed to maintain conserved quantities of the flow in afinite-volume sense. Divergence-free magnetic field topologies aremaintained to machine precision by collating the components of themagnetic field on a cell-interface staggered grid and utilizing theconstrained transport approach for integrating the induction equations.The maintenance of magnetic field topologies on adaptive grids isachieved using prolongation and restriction operators which preserve thedivergence and curl of the magnetic field across collocated grids ofdifferent resolutions. The robustness and correctness of the code isdemonstrated by comparing the numerical solution of various tests withanalytical solutions or previously published numerical solutionsobtained by other codes.},
    archivePrefix = {arXiv},
    author = {Cunningham, A. J. and Frank, A. and Varni\`{e}re, P. and Mitran, S. and Jones, T. W.},
    citeulike-article-id = {2776532},
    citeulike-linkout-0 = {http://arxiv.org/abs/0710.0424},
    citeulike-linkout-1 = {http://arxiv.org/pdf/0710.0424},
    citeulike-linkout-2 = {http://dx.doi.org/10.1088/0067-0049/182/2/519},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2007arXiv0710.0424C},
    doi = {10.1088/0067-0049/182/2/519},
    eprint = {0710.0424},
    journal = {\apjs},
    keywords = {2009, andy, astrobear},
    month = {June},
    pages = {519--542},
    posted-at = {2009-09-17 23:30:40},
    priority = {2},
    title = {Simulating Magnetohydrodynamical Flow with Constrained Transport and Adaptive Mesh Refinement: Algorithms and Tests of the AstroBEAR Code},
    url = {http://dx.doi.org/10.1088/0067-0049/182/2/519},
    volume = {182},
    year = {2009}
}



@article{jonathan2009,
    abstract = {In this paper, we explore the relationship between protostellar outflowsand turbulence in molecular clouds. Using three-dimensional numericalsimulations we focus on the hydrodynamics of multiple outflowsinteracting within a parsec scale volume. We explore the extent to whichtransient outflows injecting directed energy and momentum into asubvolume of a molecular cloud can be converted into random turbulentmotions. We show that turbulence can readily be sustained by theseinteractions and it is possible to broadly characterize an effectivedriving scale of the outflows. We compare the velocity spectrum obtainedin our studies with that of isotropically forced hydrodynamic turbulencefinding that in outflow-driven turbulence a power law of the form E(k)vprop k <SUP>--beta</SUP> is indeed achieved. However, we findthat a steeper spectrum beta \~{} 2.74 is obtained in outflow-driventurbulence models than in isotropically forced simulations beta \~{}2.45. We discuss possible physical mechanisms responsible for theseresults as well as their implications for turbulence in molecular cloudswhere outflows will act in concert with other processes such asgravitational collapse.},
    archivePrefix = {arXiv},
    author = {Carroll, J. J. and Frank, A. and Blackman, E. G. and Cunningham, A. J. and Quillen, A. C.},
    citeulike-article-id = {5800732},
    citeulike-linkout-0 = {http://arxiv.org/abs/0805.4645},
    citeulike-linkout-1 = {http://arxiv.org/pdf/0805.4645},
    citeulike-linkout-2 = {http://dx.doi.org/10.1088/0004-637X/695/2/1376},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2009ApJ...695.1376C},
    doi = {10.1088/0004-637X/695/2/1376},
    eprint = {0805.4645},
    journal = {\apj},
    keywords = {2009, turbulence},
    month = {April},
    pages = {1376--1381},
    posted-at = {2009-09-17 23:29:09},
    priority = {2},
    title = {Outflow-Driven Turbulence in Molecular Clouds},
    url = {http://dx.doi.org/10.1088/0004-637X/695/2/1376},
    volume = {695},
    year = {2009}
}



@article{truelove1998,
    abstract = {We describe a new code for numerical solution of three-dimensionalself-gravitational hydrodynamics problems. This code utilizes thetechnique of local adaptive mesh refinement (AMR), employing multiplegrids at multiple levels of resolution and automatically and dynamicallyadding and removing these grids as necessary to maintain adequateresolution. This technology allows solution of problems that would beprohibitively expensive with a code using fixed resolution, and it ismore versatile and efficient than competing methods of achievingvariable resolution. In particular, we apply this technique to simulatethe collapse and fragmentation of a molecular cloud, a key step in starformation. The simulation involves many orders of magnitude of variationin length scale as fragments form at positions that are not a prioridiscernible from general initial conditions. In this paper, we describethe methodology behind this new code and present several illustrativeapplications. The criterion that guides the degree of adaptive meshrefinement is critical to the success of the scheme, and, for theisothermal problems considered here, we employ the Jeans condition forthis purpose. By maintaining resolution finer than the local Jeanslength, we set new benchmarks of accuracy by which to measure othercodes on each problem we consider, including the uniform collapse of afinite pressured cloud. We find that the uniformly rotating, sphericalclouds treated here first collapse to disks in the equatorial plane andthen, in the presence of applied perturbations, form filamentarysingularities that do not fragment while isothermal. Our results providenumerical confirmation of recent work by Inutsuka \& Miyama on thisscenario of isothermal filament formation.},
    author = {{Truelove}, J. K. and Klein, R. I. and McKee, C. F. and Holliman, J. H. and Howell, L. H. and Greenough, J. A. and Woods, D. T.},
    citeulike-article-id = {5800724},
    citeulike-linkout-0 = {http://dx.doi.org/10.1086/305329},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1998ApJ...495..821T},
    doi = {10.1086/305329},
    journal = {\apj},
    keywords = {1998, self-gravity},
    month = {March},
    posted-at = {2009-09-17 23:23:43},
    priority = {2},
    title = {Self-gravitational Hydrodynamics with Three-dimensional Adaptive Mesh Refinement: Methodology and Applications to Molecular Cloud Collapse and Fragmentation},
    url = {http://dx.doi.org/10.1086/305329},
    volume = {495},
    year = {1998}
}



@article{pittard2009,
    abstract = {The interaction of a shock with a cloud has been extensively studied inthe literature, where the effects of magnetic fields, radiative coolingand thermal conduction have been considered. In many cases, theformation of fully developed turbulence has been prevented by theartificial viscosity inherent in hydrodynamical simulations. Thisproblem is particularly severe in some recent simulations designed toinvestigate the interaction of a flow with multiple clouds, where theresolution of individual clouds is necessarily poor. Furthermore, theshocked flow interacting with the cloud has been assumed to becompletely uniform in all previous single-cloud studies. In reality, theflow behind the shock is also likely to be turbulent, with non-uniformdensity, pressure and velocity structure created as the shock sweepsover inhomogeneities upstream of the cloud (as seen in recent multiplecloud simulations). To address these twin issues we use a subgridcompressible k-ε turbulence model to estimate the properties ofthe turbulence generated in shock-cloud interactions and the resultingincrease in the transport coefficients that the turbulence brings. Adetailed comparison with the output from an inviscid hydrodynamical codeputs these new results into context.<p/>Despite the above concerns, we find that cloud destruction in inviscidand k-ε models occurs at roughly the same speed when thepost-shock flow is smooth and when the density contrast between thecloud and intercloud medium, chi <\~{} 100. However, there areincreasing and significant differences as chi increases. Thek-ε models also demonstrate better convergence in resolutiontests than inviscid models, a feature which is particularly useful formultiple-cloud simulations.<p/>Clouds which are over-run by a highly turbulent post-shock environmentare destroyed significantly quicker as they are subject to strong`buffeting' by the flow. The decreased lifetime and faster accelerationof the cloud material to the speed of the ambient flow leads to areduction in the total amount of circulation (vorticity) generated inthe interaction, so that the amount of vorticity may be self-limiting.Additional calculations with an inviscid code where the post-shock flowis given random, grid-scale, motions confirm the more rapid destructionof the cloud.<p/>Our results clearly show that turbulence plays an important role inshock-cloud interactions, and that environmental turbulence adds a newdimension to the parameter space which has hitherto been studied.},
    archivePrefix = {arXiv},
    author = {Pittard, J. M. and Falle, S. A. E. G. and Hartquist, T. W. and Dyson, J. E.},
    citeulike-article-id = {4272378},
    citeulike-linkout-0 = {http://arxiv.org/abs/0807.4402},
    citeulike-linkout-1 = {http://arxiv.org/pdf/0807.4402},
    citeulike-linkout-2 = {http://dx.doi.org/10.1111/j.1365-2966.2009.13759.x},
    citeulike-linkout-3 = {http://www.ingentaconnect.com/content/bsc/mnr/2009/00000394/00000003/art00014},
    citeulike-linkout-4 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2009MNRAS.394.1351P},
    doi = {10.1111/j.1365-2966.2009.13759.x},
    eprint = {0807.4402},
    issn = {0035-8711},
    journal = {\mnras},
    keywords = {2009, clumps},
    month = {April},
    number = {3},
    pages = {1351--1378},
    posted-at = {2009-09-17 23:21:30},
    priority = {2},
    publisher = {Blackwell Publishing},
    title = {The turbulent destruction of clouds - I. A k-{$\epsilon$} treatment of turbulence in 2D models of adiabatic shock-cloud interactions},
    url = {http://dx.doi.org/10.1111/j.1365-2966.2009.13759.x},
    volume = {394},
    year = {2009}
}

@ARTICLE{calder2002,
   author = {{Calder}, A.~C. and {Fryxell}, B. and {Plewa}, T. and {Rosner}, R. and 
        {Dursi}, L.~J. and {Weirs}, V.~G. and {Dupont}, T. and {Robey}, H.~F. and 
        {Kane}, J.~O. and {Remington}, B.~A. and {Drake}, R.~P. and 
        {Dimonte}, G. and {Zingale}, M. and {Timmes}, F.~X. and {Olson}, K. and 
        {Ricker}, P. and {MacNeice}, P. and {Tufo}, H.~M.},
    title = "{On Validating an Astrophysical Simulation Code}",
  journal = {\apjs},
   eprint = {arXiv:astro-ph/0206251},
 keywords = {Hydrodynamics, Instabilities, Methods: Numerical, Shock Waves},
     year = 2002,
    month = nov,
   volume = 143,
    pages = {201-229},
      doi = {10.1086/342267},
   adsurl = {http://adsabs.harvard.edu/abs/2002ApJS..143..201C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}


@ARTICLE{hartigan2009,
   author = {{Hartigan}, P. and {Foster}, J.~M. and {Wilde}, B.~H. and {Coker}, R.~F. and 
        {Rosen}, P.~A. and {Hansen}, J.~F. and {Blue}, B.~E. and {Williams}, R.~J.~R. and 
        {Carver}, R. and {Frank}, A.},
    title = "{Laboratory Experiments, Numerical Simulations, and Astronomical Observations of Deflected Supersonic Jets: Application to HH 110}",
  journal = {\apj},
archivePrefix = "arXiv",
   eprint = {0910.0318},
 keywords = {hydrodynamics, ISM: Herbig-Haro objects, ISM: jets and outflows, methods: laboratory, shock waves},
     year = 2009,
    month = nov,
   volume = 705,
    pages = {1073-1094},
      doi = {10.1088/0004-637X/705/1/1073},
   adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...705.1073H},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{kim2009sf,
   author = {{Kim}, {J.-h.} and {Wise}, J.~H. and {Abel}, T.},
    title = "{Galaxy Mergers with Adaptive Mesh Refinement: Star Formation and Hot Gas Outflow}",
  journal = {\apjl},
archivePrefix = "arXiv",
   eprint = {0902.3001},
 keywords = {galaxies: formation, galaxies: interactions, galaxies: starburst, stars: formation},
     year = 2009,
    month = apr,
   volume = 694,
    pages = {L123-L127},
      doi = {10.1088/0004-637X/694/2/L123},
   adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...694L.123K},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{greif2007sn,
   author = {{Greif}, T.~H. and {Johnson}, J.~L. and {Bromm}, V. and {Klessen}, R.~S.
        },
    title = "{The First Supernova Explosions: Energetics, Feedback, and Chemical Enrichment}",
  journal = {\apj},
archivePrefix = "arXiv",
   eprint = {0705.3048},
 keywords = {Cosmology: Theory, Galaxies: Formation, Galaxies: High-Redshift, ISM: H II Regions, Hydrodynamics, Galaxies: Intergalactic Medium, Stars: Supernovae: General},
     year = 2007,
    month = nov,
   volume = 670,
    pages = {1-14},
      doi = {10.1086/522028},
   adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...670....1G},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@article{kleinwoods1998,
    abstract = {A fundamental problem in interstellar gasdynamics is the collisionbetween two interstellar clouds. We present high-resolutiontwo-dimensional results of this interaction using Adaptive meshrefinement (AMR) hydrodynamics with a Godunov scheme for accurate shocktracking in multidimensions. These results are at a resolution that issignificantly higher than has been previously achieved by othermethodologies such as smoothed particle hydrodynamics. We have studiedthe collisions between homogeneous clouds with an adiabatic equation ofstate, isothermal clouds, radiatively cooling clouds, and clouds withinitial surface perturbations. In all instances, the collision iscomplex, resulting in flows that are strongly influenced byKelvin-Helmholtz and nonlinear thin shell bending mode instabilities. Inparticular we find that the early evolution of homogeneous cloudcollisions initially produces a cold dense disk in the collisionmidplane. A low mass jet propagates outward with characteristics ofdense protostellar jets in a low-density medium. Once the clouds havebeen compressed by strong shocks, pressure gradients drive the densedisk to re-expand along the symmetry axis. This reexpansion overshoots,resulting in a pressure deficit in the interior of the merged cloudsystem and a collapse back onto the symmetry axis. If the collidingclouds are initially smooth, the end result of the collision is a largeaspect ratio filament with a homogeneous interior and an irregularsurface. If the clouds have finite surface perturbations, a bending modeinstability renders the merged cloud system asymmetrical and highlyinhomogeneous with islands of high density surrounded by low densityregions throughout the interior. These results have implications forcoelescence models of star formation. The appearance of the mergedsystem is that of a clumpy filamentary structure with a large aspectratio. This instability is shown to occur for both isothermal shocks, aswell as shocks with radiative cooling. The instability occurs inadiabatic shocks for compressions greater than 10. The bending modeinstability increases the vorticity of the merged cloud system,resulting in an axial velocity that is twice as large as in the smoothcloud case. Recent observations show an abundance of elongated clumpyfilaments in the Orion Molecular Cloud (OMC-1). Our calculations ofcloud-cloud collisions undergoing the bending mode instability provide anew mechanism for for generating inhomogeneous filamentary structureswhich appear to be common in the interstellar medium.},
    author = {Klein, R. I. and Woods, D. T.},
    citeulike-article-id = {5800720},
    citeulike-linkout-0 = {http://dx.doi.org/10.1086/305488},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1998ApJ...497..777K},
    doi = {10.1086/305488},
    journal = {\apj},
    keywords = {1998, clumps},
    month = {April},
    posted-at = {2009-09-17 23:20:12},
    priority = {2},
    title = {Bending Mode Instabilities and Fragmentation in Interstellar Cloud Collisions: A Mechanism for Complex Structure},
    url = {http://dx.doi.org/10.1086/305488},
    volume = {497},
    year = {1998}
}



@article{shin2008,
    abstract = {The magnetohydrodynamic evolution of a dense spherical cloud as itinteracts with a strong planar shock is studied, as a model for shockinteractions with density inhomogeneities in the interstellar medium.The cloud is assumed to be small enough that radiative cooling, thermalconduction, and self-gravity can be ignored. A variety of initialorientations (including parallel, perpendicular, and oblique to theincident shock normal) and strengths for the magnetic field areinvestigated. During the early stages of the interaction (less thantwice the time taken for the transmitted shock to cross the interior ofthe cloud), the structure and dynamics of the shocked cloud are fairlyinsensitive to the magnetic field strength and orientation. However, atlate times strong fields substantially alter the dynamics of the cloud,suppressing fragmentation and mixing by stabilizing the interface at thecloud surface. Even weak magnetic fields can drastically alter theevolution of the cloud compared to the hydrodynamic case. Weak fields ofdifferent geometries result in different distributions andamplifications of the magnetic energy density, which may affect thethermal and nonthermal X-ray emission expected from shocked cloudsassociated with, for example, supernova remnants.},
    archivePrefix = {arXiv},
    author = {Shin, M. S. and Stone, J. M. and Snyder, G. F.},
    citeulike-article-id = {5800715},
    citeulike-linkout-0 = {http://arxiv.org/abs/0802.2708},
    citeulike-linkout-1 = {http://arxiv.org/pdf/0802.2708},
    citeulike-linkout-2 = {http://dx.doi.org/10.1086/587775},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2008ApJ...680..336S},
    doi = {10.1086/587775},
    eprint = {0802.2708},
    journal = {\apj},
    keywords = {2008, clumps},
    month = {June},
    pages = {336--348},
    posted-at = {2009-09-17 23:17:02},
    priority = {2},
    title = {The Magnetohydrodynamics of Shock-Cloud Interaction in Three Dimensions},
    url = {http://dx.doi.org/10.1086/587775},
    volume = {680},
    year = {2008}
}



@article{stone1992,
    abstract = {The 3D hydrodynamic evolution of a spherical bubble embedded in a lessdense uniform ambient medium is described as it interacts with a Mach-10planar shock. This scenario is an idealized model of the interaction ofan interstellar cloud with a large supernova remnant. A third-orderGodunov numerical algorithm and 5.2 x 10 exp 6 grid points are used toresolve the complex flowfield which results. The vortex rings observedin 2D simulations are unstable in three dimensions, and the cloudfragments in all directions. Turbulent mixing of the cloud andinterstellar medium is complete and is characterized by the formation ofmacroscopic vortex filaments. The strongest vortex filaments observed inour simulation are thought to be responsible for the radio emissionpeaks observed in young supernova remnants.},
    author = {Stone, J. M. and Norman, M. L.},
    citeulike-article-id = {5800711},
    citeulike-linkout-0 = {http://dx.doi.org/10.1086/186361},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1992ApJ...390L..17S},
    doi = {10.1086/186361},
    journal = {\apj},
    keywords = {1992, clumps},
    month = {May},
    pages = {L17--L19},
    posted-at = {2009-09-17 23:15:11},
    priority = {2},
    title = {The three-dimensional interaction of a supernova remnant with an interstellar cloud},
    url = {http://dx.doi.org/10.1086/186361},
    volume = {390},
    year = {1992}
}


@article{orlando2005,
    abstract = {We model the hydrodynamic interaction of a shock wave of an evolvedsupernova remnant with a small interstellar gas cloud like the onesobserved in the Cygnus loop and in the Vela SNR. We investigate theinterplay between radiative cooling and thermal conduction during cloudevolution and their effect on the mass and energy exchange between thecloud and the surrounding medium. Through the study of two casescharacterized by different Mach numbers of the primary shock (M= 30 and50, corresponding to a post-shock temperature T\&ap; 1.7×10<SUP>6</SUP> K and \&ap; 4.7× 10<SUP>6</SUP> K, respectively), weexplore two very different physical regimes: for M= 30, the radiativelosses dominate the evolution of the shocked cloud which fragments intocold, dense, and compact filaments surrounded by a hot corona which isablated by the thermal conduction; instead, for M= 50, the thermalconduction dominates the evolution of the shocked cloud, whichevaporates in a few dynamical time-scales. In both cases we find thatthe thermal conduction is very effective in suppressing the hydrodynamicinstabilities that would develop at the cloud boundaries.},
    archivePrefix = {arXiv},
    author = {Orlando, S. and Peres, G. and Reale, F. and Bocchino, F. and Rosner, R. and Plewa, T. and Siegel, A.},
    citeulike-article-id = {5800708},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0508638},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0508638},
    citeulike-linkout-2 = {http://dx.doi.org/10.1051/0004-6361:20052896},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2005A\&amp;A...444..505O},
    doi = {10.1051/0004-6361:20052896},
    eprint = {astro-ph/0508638},
    journal = {\aap},
    keywords = {2005, clumps},
    month = {December},
    pages = {505--519},
    posted-at = {2009-09-17 23:03:54},
    priority = {2},
    title = {Crushing of interstellar gas clouds in supernova remnants. I. The role of thermal conduction and radiative losses},
    url = {http://dx.doi.org/10.1051/0004-6361:20052896},
    volume = {444},
    year = {2005}
}


@article{mellema2002,
    abstract = {This letter presents a numerical study of the evolution of an emissionline cloud of initial density 10 cm<SUP>-3</SUP>, temperature10<SUP>4</SUP> K, and size 200 pc, being overtaken by a strong shockwave. Whereas previous simple models proposed that such a cloud wouldeither be completely destroyed, or simply shrink in size, our resultsshow a different and more complex behaviour: due to rapid cooling, thecloud breaks up into many small and dense fragments, which can survivefor a long time. We show that such rapid cooling behaviour is expectedfor a wide range of cloud and shock properties. This process applies tothe evolution of emission line clouds being overtaken by the cocoon of aradio jet. The resulting small clouds would be Jeans unstable, and formstars. Our results thus give theoretical credibility to the process ofjet induced star formation, one of the explanations for the alignment ofthe optical/UV and radio axis observed in high redshift radio galaxies.},
    archivePrefix = {arXiv},
    author = {Mellema, G. and Kurk, J. D. and R\"{o}ttgering, H. J. A.},
    citeulike-article-id = {5800695},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0209601},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0209601},
    citeulike-linkout-2 = {http://dx.doi.org/10.1051/0004-6361:20021408},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2002A\&amp;A...395L..13M},
    doi = {10.1051/0004-6361:20021408},
    eprint = {astro-ph/0209601},
    journal = {\aap},
    keywords = {2002, clumps},
    month = {November},
    pages = {L13--L16},
    posted-at = {2009-09-17 22:50:51},
    priority = {2},
    title = {Evolution of clouds in radio galaxy cocoons},
    url = {http://dx.doi.org/10.1051/0004-6361:20021408},
    volume = {395},
    year = {2002}
}

@article{falle1987,
        abstract = {This paper contains some results of axisymmetric numerical calculations
of the shock structures in steady supersonic jets in which there is
significant radiative cooling. It is found that the regularly spaced
shock cells found in adiabatic jets still occur and that cooling can by
itself induce shocks if it is fast enough. The forbidden O I line
emission from such jets is calculated and compared to that seen in
stellar jets. The pattern of emission is very similar to that observed,
which suggests that a number of the features of stellar jets can be
understood in this way.},
        author = {Falle, S. A. E. G.  and Innes, D. E.  and Wilson, M. J. },
        citeulike-article-id = {3731393},
        journal = {\mnras},
        keywords = {1987},
        month = {April},
        pages = {741--759},
        posted-at = {2008-12-01 02:01:36},
        priority = {2},
        title = {Steady stellar jets},
        url = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1987MNRAS.225..741F},
        volume = {225},
        year = {1987}
}


@article{vitorino2002,
        abstract = {We study the outflows from randomly perturbed Keplerian accretion disks. In the velocity field of the gas at the surface of the disk, we introduce a random perturbation proportional to r<SUP>a</SUP>, where r is the radial distance and a is a fixed parameter in the simulation (with values of -3/2, -1, -1/2, 0, 1/2 or 1). In the simulations, the disk is a fixed boundary from which the gas is ejected with continuous and random velocities added together. The continuous ejection velocity is taken to be a thousandth of that of the local Keplerian disk; the maximum value of the random velocity is 10 times the continuous velocity. We observe the formation of periodic structures along the outflow axis. The distance of the axial separation between the structures is found to be about 11 times the innermost radius of the accretion disk. For a negative radial slope a, the structures are well defined and situated near the jet axis, whereas for a positive slope, decollimation of the jet occurs.},
        author = {Vitorino, B. F.  and Jatenco-Pereira, V.  and Opher, R. },
        citeulike-article-id = {3731390},
        doi = {http://dx.doi.org/10.1051/0004-6361:20011726},
        journal = {\aap},
        keywords = {2002},
        month = {March},
        pages = {329--342},
        posted-at = {2008-12-01 01:57:02},
        priority = {2},
        title = {Numerical simulations of astrophysical jets from randomly perturbed Keplerian disks},
        url = {http://dx.doi.org/10.1051/0004-6361:20011726},
        volume = {384},
        year = {2002}
}



@article{dalpino1994,
        abstract = {We present fully three-dimensional simulations of supersonic, radiatively cooling intermitten jets with intermediate and long variability periods. Variations of intermediate period elucidate the formation and evolution of chains of internal regularly spaced radiative shocks, which in this work are identified with the observed emission knots of protostellar jets. Variations of long period elucidate the formation of multiple bow shock structures separated by long trails of diffuse gas, which resemble those observed in systems like HH 111 and HH 46/47. The time variability of the outflow is probably associated with observed irruptive events in the accretion process around the protostars. In our simulations the outflow variations are produced by periodically turning on the outflow with a highly supersonic velocity and periodically turning off it to a low-velocity regime. When a supersonic parcel finds the flow material that has been ejected earlier, a double shock structure promptly develops: a forward shock sweeps up the slow material ahead of it and a reverse shock decelerates the fast material behind. The very high density contrast between the fast and slow portions of the flow causes the reverse shock to be much weaker than the forward shock so that line emission by gas between these shocks is essentially single peaked. In the case of velocity variations of intermediate period, we find that the shock structures form a train of regularly spaced emitting features which move away from the source with a velocity close to that of the outflow, have high radial motions, and produce low-intensity spectra, as required by the observations. In the case of the long-period velocity variability, our simulations have produced a pair of bowshock-like structures separated by a trail almost starved of gas extending for many jet radii in agreement with the observations. A brief discussion on the possibility of these time-dependent intermittent jets to drive molecular outflows is also presented.},
        author = {de Gouveia Dal Pino, E. M. and Benz, W. },
        citeulike-article-id = {3731364},
        doi = {http://dx.doi.org/10.1086/174811},
        eprint = {astro-ph/9405035},
        journal = {\apj},
        keywords = {1994, de-gouveia-dal-pino},
        month = {November},
        pages = {261--273},
        posted-at = {2008-12-01 01:39:32},
        priority = {2},
        title = {Multiple outflow episodes from protostars: Three-dimensional models of intermittent jets},
        url = {http://dx.doi.org/10.1086/174811},
        volume = {435},
        year = {1994}
}



@article{cerqueira2006,
        abstract = {Using the Yguaz\'{u}-a three-dimensional hydrodynamic code, we have computed a set of numerical simulations of heavy, supersonic, radiatively cooling jets including variabilities in both the ejection direction (precession) and the jet velocity (intermittence). In order to investigate the effects of jet rotation on the shape of the line profiles, we also introduce an initial toroidal rotation velocity profile, in agreement with some recent observational evidence found in jets from T Tauri stars which seems to support the presence of a rotation velocity pattern inside the jet beam, near the jet production region. Since the Yguaz\'{u}-a code includes an atomic/ionic network, we are able to compute the emission coefficients for several emission lines, and we generate line profiles for the Halpha, [O I]lambda6300, [S II]lambda6716 and [N II]lambda6548 lines. Using initial parameters that are suitable for the DG Tau microjet, we show that the computed radial velocity shift for the medium-velocity component of the line profile as a function of distance from the jet axis is strikingly similar for rotating and non-rotating jet models. These findings lead us to put forward some caveats on the interpretation of the observed radial velocity distribution from a few outflows from young stellar objects, and we claim that these data should not be directly used as a doubtless confirmation of the magnetocentrifugal wind acceleration models.},
        author = {Cerqueira, A. H.  and Vel\'{a}zquez, P. F.  and Raga, A. C.  and Vasconcelos, M. J.  and de Colle, F. },
        citeulike-article-id = {3731336},
        doi = {http://dx.doi.org/10.1051/0004-6361:20054110},
        eprint = {astro-ph/0510572},
        journal = {\aap},
        keywords = {2006},
        month = {March},
        pages = {231--241},
        posted-at = {2008-12-01 00:58:53},
        priority = {2},
        title = {Emission lines from rotating proto-stellar jets with variable velocity profiles. I. Three-dimensional numerical simulation of the non-magnetic case},
        url = {http://dx.doi.org/10.1051/0004-6361:20054110},
        volume = {448},
        year = {2006}
}



@article{hartigan2001,
        abstract = {New Halpha and [S II] images of the HH 111 jet taken with the Hubble Space Telescope reveal marked proper motions and morphological changes when compared with similar images obtained 4 years earlier. Knots in the jet, which are dominated by emission from nested bow shocks, generally move ballistically, with no evidence for turbulent motions even in regions where the emission has a complex morphology. These bow shocks sometimes overtake one another; the new images show this occurred in knot L about 80 years ago. Photometric variability, clearly visible for the first time at subarcsecond scales, can confuse ground-based measurements that require many years between epochs to detect reliable proper motions. With the exception of the bow shock L, whose wings expand laterally, the jet moves mainly along its long axis. Because HH 111 lies nearly in the plane of the sky, the proper motions translate accurately to space velocities, which range from 220 to 330 km s<SUP>-1</SUP> with a typical uncertainty of +/-5 km s<SUP>-1</SUP>. The fastest knots are associated with object E at the base of the visible jet, where a cooling layer is in the process of forming behind one of the shocks. Velocity differences between adjacent knots within the optically bright part of the jet are typically 40 km s<SUP>-1</SUP>, in line with predictions of nonmagnetic shock models based on emission-line fluxes. This agreement limits the component of the magnetic field perpendicular to the axis of the jet to be <\~{}1 mG. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.},
        author = {Hartigan, P.  and Morse, J. A.  and Reipurth, B.  and Heathcote, S.  and Bally, J. },
        citeulike-article-id = {3731277},
        doi = {http://dx.doi.org/10.1086/323976},
        journal = {\apj},
        keywords = {2001, hh-111},
        month = {October},
        pages = {L157--L161},
        posted-at = {2008-11-30 23:20:30},
        priority = {2},
        title = {Proper Motions of the HH 111 Jet Observed with the Hubble Space Telescope},
        url = {http://dx.doi.org/10.1086/323976},
        volume = {559},
        year = {2001}
}



@article{riera2003,
        abstract = {We present long-slit spectroscopic observations of the HH 110 jet obtained with the 4.2 m William Herschel Telescope. We have obtained for the first time, spectra for slit positions along and across the jet axis (at the position of knots B, C, I, J and P) to search for the observational signatures of entrainment and turbulence by studying the kinematics and the excitation structure. We find that the HH 110 flow accelerates from a velocity of 35 km s<SUP>-1</SUP> in knot A up to 110 km s<SUP>-1</SUP> in knot P. We find some systematic trends for the variation of the emission line ratios along the jet. No clear trends for the variation of the radial velocity are seen across the width of the jet beam. The cross sections of the jet show complex radial velocity and line emission structures which differ quite strongly from each other.<p> Based on observations made with the 4.2 m William Herschel Telescope operated on La Palma by the Issac Newton Group of Telescopes at the Observatorio del Roque de los Muchachos of the Instituto de Astrof\'{i}sica de Canarias.},
        author = {Riera, A.  and L\'{o}pez, R.  and Raga, A. C.  and Estalella, R.  and Anglada, G. },
        citeulike-article-id = {3729954},
        doi = {http://dx.doi.org/10.1051/0004-6361:20021879},
        eprint = {astro-ph/0302059},
        journal = {\aap},
        keywords = {2003, hh-110},
        month = {March},
        pages = {213--221},
        posted-at = {2008-11-30 19:39:08},
        priority = {2},
        title = {The transverse velocity and excitation structure of the HH 110 jet},
        url = {http://dx.doi.org/10.1051/0004-6361:20021879},
        volume = {400},
        year = {2003}
}



@article{riera2001,
        abstract = {We present long-slit spectroscopic observations of the HH 111 jet obtained with the 4.2 m William Herschel Telescope. We have obtained spectra for slit positions along and across the jet axis, in order to search for radial velocity, electron density and excitation variations across the jet. We have detected faint emission across knots HH 111 D and F, extending to large (\~{} 15”) distances from the flow axis. This extended emission shows a radial velocity stratification, with higher radial velocities on the jet axis and lower velocities away from the axis. Knot D has a low central electron density surrounded by material with higher electron densities, while the electron density is approximately constant across knot F. We argue that the extended emission and the radial velocity variations observed across the HH 111 flow are compatible with a jet beam with a transverse gradient in velocity or with a jet which is entraining low velocity material.},
        author = {Riera, A.  and L\'{o}pez, R.  and Raga, A. C.  and Anglada, G.  and Estalella, R. },
        citeulike-article-id = {3729951},
        journal = {RevMexAA},
        keywords = {2001, hh-111},
        month = {October},
        pages = {147--157},
        posted-at = {2008-11-30 19:38:41},
        priority = {2},
        title = {The Transverse Velocity Structure of the HH 111 Jet},
        url = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2001RMxAA..37..147R},
        volume = {37},
        year = {2001}
}


@article{payne1985,
        abstract = {The linear stability of a confined radio jet is reinvestigated. The roles of both absolute (temporal) and convected (spatial) instability are considered, and it is demonstrated that the two are related through the group velocity. The dispersion relation is analyzed asymptotically for the fundamental and reflection modes. Numerical results are presented for pinching modes. A geometrical interpretation of the modes is presented in terms of the propagation angle and is visualized by contour plots of the pressure perturbation. A confined jet theta M = arc sine (1 + sq rt eta)/M, where eta is the ratio of the internal to the external gas density and M is the Mach number of the jet. The connection between these linear modes and the cross-shaped shock patterns which are seen in laboratory jets, and the implications of these calculations for the development of large-scale features in extragalactic radio jets, are discussed.},
        author = {Payne, D. G.  and Cohn, H. },
        citeulike-article-id = {3709371},
        doi = {http://dx.doi.org/10.1086/163104},
        journal = {\apj},
        keywords = {1985},
        month = {April},
        pages = {655--667},
        posted-at = {2008-11-26 21:19:14},
        priority = {2},
        title = {The stability of confined radio jets - The role of reflection modes},
        url = {http://dx.doi.org/10.1086/163104},
        volume = {291},
        year = {1985}
}

@article{dalpino1993,
        abstract = {We present the first results of fully 3D simulations of supersonic, radiatively cooling jets using the smoothed particle hydrodynamics technique (SPH). Our results qualitatively agree with the 2D simulations of Blondin et al. (1990), although the removal of the axisymmetry has resulted in relevant structural differences, especially at the jet head where a cold shell is formed from the condensation of shock-heated material. In particular, we found that the shell is not only dynamically unstable but also may undergo oscillations in density, which are attributed to global thermal instabilities. These effects may have important consequences on the dynamics and emission pattern of the observed HH objects associated to young stellar jets. We discuss the implications of our results in the interpretation of the observed properties of the stellar jets and HH objects. We also compare the structure of radiative cooling and adiabatic 3D jets.},
        author = {de Gouveia Dal Pino, E. M. and Benz, W. },
        citeulike-article-id = {3709335},
        doi = {http://dx.doi.org/10.1086/172785},
        journal = {\apj},
        keywords = {1993, de-gouveia-dal-pino},
        month = {June},
        pages = {686--695},
        posted-at = {2008-11-26 20:56:51},
        priority = {2},
        title = {Three-dimensional simulations of protostellar jets},
        url = {http://dx.doi.org/10.1086/172785},
        volume = {410},
        year = {1993}
}



@article{thiele2002,
        abstract = {We present the results of a simulation of an axisymmetric (2.5-dimensional), magnetized Herbig-Haro jet. The parameters are chosen for a typical collimated outflow from a young stellar low-mass object. We show that the nose-cone feature of 2D MHD jets critically depends on the magnetic field topology of the precollimation mechanism. The most prominent features of our model jet are knot-like structures along the jet axis which develop in the foremost part of the jet. Shocks associated with these internal knot-like structures mimic bow-shock like features as seen in Herbig-Haro flows.},
        author = {Thiele, M.  and Camenzind, M. },
        citeulike-article-id = {3709331},
        doi = {http://dx.doi.org/10.1051/0004-6361:20011652},
        journal = {\aap},
        keywords = {2002},
        month = {January},
        pages = {L53--L56},
        posted-at = {2008-11-26 20:55:19},
        priority = {2},
        title = {Knot production in magnetized Herbig-Haro jets},
        url = {http://dx.doi.org/10.1051/0004-6361:20011652},
        volume = {381},
        year = {2002}
}

@article{ciardi2008,
        abstract = {Collimated outflows (jets) are ubiquitous in the universe appearing around sources as diverse as protostars and extragalactic supermassive blackholes. Jets are thought to be magnetically collimated, and launched from a magnetized accretion disk surrounding a compact gravitating object. We have developed the first laboratory experiments to address time-dependent, episodic phenomena relevant to the poorly understood jet acceleration and collimation region. The experimental results show the periodic ejections of magnetic bubbles naturally evolving into a heterogeneous jet propagating inside a channel made of self-collimated magnetic cavities. The results provide a unique view of the possible transition from a relatively steady-state jet launching to the observed highly structured outflows.},
        author = {Ciardi, A.  and Lebedev, S. V.  and Frank, A.  and Suzuki-Vidal, F.  and Hall, G. N.  and Bland, S. N.  and Harvey-Thompson, A.  and Blackman, E. G.  and Camenzind, M. },
        citeulike-article-id = {3708947},
        eprint = {0811.2736},
        journal = {ArXiv:astro-ph/0811.2736},
        keywords = {2008, lab},
        month = {November},
        posted-at = {2008-11-26 18:53:42},
        priority = {2},
        title = {Episodic Magnetic Bubbles and Jets: Astrophysical Implications from Laboratory Experiments},
        url = {http://arxiv.org/abs/0811.2736},
        volume = {811},
        year = {2008}
}

@ARTICLE{anathpindika2009,
   author = {{Anathpindika}, S.},
    title = "{Supersonic cloud collision. I.}",
  journal = {\aap},
archivePrefix = "arXiv",
   eprint = {0810.5011},
 keywords = {hydrodynamics, shock waves, ISM: clouds, instabilities, star: formation},
     year = 2009,
    month = sep,
   volume = 504,
    pages = {437-450},
      doi = {10.1051/0004-6361/200911748},
   adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...504..437A},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@ARTICLE{miniati2c1999,
   author = {{Miniati}, F. and {Ryu}, D. and {Ferrara}, A. and {Jones}, T.~W.
        },
    title = "{Magnetohydrodynamics of Cloud Collisions in a Multiphase Interstellar Medium}",
  journal = {\apj},
   eprint = {arXiv:astro-ph/9808174},
 keywords = {ISM: CLOUDS, ISM: KINEMATICS AND DYNAMICS, MAGNETIC FIELDS, MAGNETOHYDRODYNAMICS: MHD, SHOCKWAVES},
     year = 1999,
    month = jan,
   volume = 510,
    pages = {726-746},
      doi = {10.1086/306599},
   adsurl = {http://adsabs.harvard.edu/abs/1999ApJ...510..726M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{miniati1999,
        abstract = {},
        author = {Miniati, F. and Jones, T.~W. and Ryu, D.},
        citeulike-article-id = {},
        doi = {},
        eprint = {},
        journal = {\apj},
        keywords = {1999},
        month = {},
        pages = {242},
        posted-at = {},
        priority = {},
        title = {On the Exchange of Kinetic and Magnetic Energy between Clouds and the Interstellar Medium},
        url = {},
        volume = {517},
        year = {1999}
}

@article{miniati1997,
    abstract = {We have studied head-on collisions between equal-mass, mildly supersonic H I clouds (Mach number 1.5 with respect to the background medium) through high-resolution numerical simulations in two dimensions. We explore the role of various factors, including the radiative cooling parameter, eta = tau rad/ tau coll ( tau coll = Rc/vc), evolutionary modifications on the cloud structure, and the symmetry of the problem. Self-gravity is not included. Radiative losses are taken into account explicitly and not approximated with an isothermal adiabatic index gamma \~{} 1, which, in fact, leads to very different results. We assume a standard two-phase interstellar medium (ISM) model where clouds are characterized by a temperature Tc = 74 K and number density nc = 22 cm-3 and are in pressure equilibrium with the surrounding warm intercloud medium (WIM), with a density contrast chi = rho c/ rho i = 100. In particular, we study collisions for the adiabatic ( eta >> 1) and radiative ( eta = 0.38) cases that may correspond to small (Rc <= 0.4 pc for an assumed WIM) or large (Rc \~{} 1.5 pc) clouds, respectively. In addition to a standard case of identical "nonevolved" clouds, we also consider the collision of identical clouds, "evolved" through independent motion within the intercloud gas, over one crushing time before collision. This turns out to be about the mean collision time for such clouds in the ISM. The presence of bow shocks and ram pressure from material in the cloud wake alters these interactions significantly with respect to the standard case. In some cases, we removed the mirror symmetry from the problem by colliding initially identical clouds "evolved" to different ages before impact. In those cases, the colliding clouds have different density and velocity structures, so that they provide a first insight on the behavior of more complex interactions. In our adiabatic collisions, the clouds are generally disrupted and convert their gas into the warm phase of the ISM. Although the details depend on the initial conditions, the two colliding clouds are converted into a few low-density contrast ( chi \~{} 5) clumps at the end of the simulations. By contrast, for symmetric radiative cases, we find that the two clouds coalesce, and there are good chances for a new massive cloud to be formed. Almost all the initial kinetic energy of the two clouds is radiated away during such collisions. On the other hand, for both adiabatic and radiative collisions, symmetry breaking leads to major differences. Most importantly, asymmetric collisions have a much greater tendency to disrupt the two clouds. Portions of individual clouds may be sheared away, and instabilities along the interfaces between the clouds and with the intercloud medium are enhanced. In addition, radiative cooling is less efficient in our asymmetric interactions, so that those parts of the clouds that initially seem to merge are more likely to reexpand and fade into the warm intercloud medium. Since the majority of real cloud collisions should be asymmetric for one reason or another, we conclude that most gasdynamical diffuse cloud collisions will be disruptive, at least in the absence of significant self-gravity or a significant magnetic field.},
    archivePrefix = {arXiv},
    author = {Miniati, F. and Jones, T. W. and Ferrara, A. and Ryu, D.},
    citeulike-article-id = {2862936},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/9706208},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/9706208},
    citeulike-linkout-2 = {http://dx.doi.org/10.1086/304953},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1997ApJ...491..216M},
    doi = {10.1086/304953},
    eprint = {astro-ph/9706208},
    journal = {\apj},
    keywords = {1997},
    month = {December},
    pages = {216--232},
    posted-at = {2008-06-04 23:58:47},
    priority = {2},
    title = {Hydrodynamics of Cloud Collisions in Two Dimensions: The Fate of Clouds in a Multiphase Medium},
    url = {http://dx.doi.org/10.1086/304953},
    volume = {491},
    year = {1997}
}

@article{kimura1996,
    abstract = {We have investigated collisions between clumpy molecular clouds with two-dimensional hydrodynamical simulations. We consider collisions between a typical giant molecular cloud, the GMC, and a smaller one, the SMC, both of which have disturbed clumpy structure due to internal turbulence, and follow the evolution focusing our attention on the effect of the clumpy nature of the clouds. For a given GMC, the evolution and the fate of the collision depends on the size of the SMC. If its size is small (e.g. diameter one tenth of the GMC), the SMC is able to pass through the GMC giving no serious damage to its global structure, in marked contrast with the more destructive nature of collisions between uniform clouds. In the case where the SMC is large (e.g. diameter one half of the GMC), the shocked region suffers strong perturbations due to interaction with the internal clumps and shows large distortion. The compressed SMC is finally broken into many dense gas clumps, and the GMC is seriously damaged and disrupted by the collision. In all the cases we have considered, very dense gas clumps are formed as a result of the collision. Since the mass of these clumps is well above the Jeans mass, stars will be formed triggered by the cloud collision. The results indicate that the internal clumpy structure of molecular clouds strongly affects the structure and the evolution of the colliding clouds and star formation is triggered by the cloud-cloud collision. We have compared these results with those of uniform clouds to find that the difference is very significant in the formation of dense gas clumps and the ultimate fate of the collision.},
    author = {Kimura, T. and Tosa, M.},
    citeulike-article-id = {2862935},
    journal = {\aap},
    keywords = {1996},
    month = {April},
    pages = {979--987},
    posted-at = {2008-06-04 23:57:56},
    priority = {2},
    title = {Collision of clumpy molecular clouds.},
    volume = {308},
    year = {1996}
}


@article{livio1999,
    abstract = {It is assumed that the acceleration and collimation mechanisms of jets are the same in all the classes of astrophysical objects which are observed to produce jets. These classes now include such objects as: active galactic nuclei, young stellar objects, massive X-ray binaries, low mass X-ray binaries, black hole X-ray transients, symbiotic systems, planetary nebulae, and supersoft X-ray sources. On the basis of this assumption, an attempt is made to identify the necessary ingredients for the acceleration and collimation mechanism. It is argued that: (i) jets are produced at the center of accretion disks, and are accelerated and collimated hydromagnetically, and (ii) the production of powerful jets requires a hot corona or access to an additional energy source associated with the central object. Tentative explanations for the presence of jets in some classes of objects and absence in others are given. Some critical observation that can test the ideas presented in this paper are suggested.},
    author = {Livio, Mario},
    citeulike-article-id = {2838194},
    citeulike-linkout-0 = {http://dx.doi.org/10.1016/S0370-1573(98)00102-1},
    citeulike-linkout-1 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1999PhR...311..225L},
    citeulike-linkout-2 = {http://www.sciencedirect.com/science/article/B6TVP-3W4Y1CN-D/1/eb74fc5fc111fed245a07eb436593c03},
    doi = {10.1016/S0370-1573(98)00102-1},
    journal = {Physics Reports},
    keywords = {1999},
    month = {April},
    number = {3-5},
    pages = {225--245},
    posted-at = {2008-05-27 21:03:24},
    priority = {4},
    title = {Astrophysical jets: a phenomenological examination of acceleration and collimation},
    url = {http://dx.doi.org/10.1016/S0370-1573(98)00102-1},
    volume = {311},
    year = {1999}
}


@article{nakamura2006,
    abstract = {The effect of smooth cloud boundaries on the interaction of steady planar shock waves with interstellar clouds is studied using a local adaptive mesh refinement technique with an axisymmetric Godunov hydrodynamic scheme. A three-dimensional calculation is also done to confirm the two-dimensional results. We find that smooth cloud boundaries significantly affect cloud morphology and retard cloud destruction. After shock passage, a sharp density jump forms due to velocity gradients generated in the smooth cloud boundary. We refer to this density jump as a  ” slip surface” because the velocity is sheared parallel to its surface. The formation of a slip surface leads to complete cloud destruction because of the Kelvin-Helmholtz and Rayleigh-Taylor instabilities. We construct analytic models of cloud drag and vorticity generation that compare well with the numerical results. Small shreds formed by the instabilities have significant velocity dispersions of 10\%-20\% of the ambient shock velocity. They could be related to the small cold H I clouds recently observed by Stanimirovic \& Heiles. The dependence of the velocity dispersion on region size, the so-called line width-size relation, is found to be time-dependent. In the early stages, the line width-size relation is more or less flat because of the significant small-scale fluctuations generated by the Kelvin-Helmholtz instability. In the later stages, the small-scale fluctuations tend to damp, leading to a line width that increases with size. The possibility of gravitational instability triggered by shock compression is discussed. We show that gravitational collapse can be induced in an initially uniform cloud by a radiative shock (gamma<4/3) only if it is not too strong and nonthermal motions are weak.},
    archivePrefix = {arXiv},
    author = {Nakamura, F. and Mckee, C. F. and Klein, R. I. and Fisher, R. T.},
    citeulike-article-id = {2837707},
    citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0511016},
    citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0511016},
    citeulike-linkout-2 = {http://dx.doi.org/10.1086/501530},
    citeulike-linkout-3 = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=2006ApJS..164..477N},
    doi = {10.1086/501530},
    eprint = {astro-ph/0511016},
    journal = {\apjs},
    keywords = {2006, clumps},
    month = {June},
    pages = {477--505},
    posted-at = {2008-05-27 15:50:15},
    priority = {3},
    title = {On the Hydrodynamic Interaction of Shock Waves with Interstellar Clouds. II. The Effect of Smooth Cloud Boundaries on Cloud Destruction and Cloud Turbulence},
    url = {http://dx.doi.org/10.1086/501530},
    volume = {164},
    year = {2006}
}



@article{jones1996,
        abstract = {<img src="http://adsabs.harvard.edu/articles/abstracts/1996/ApJ../1996ApJ...473..365J.gif"><p>},
        author = {Jones, T. W.  and Ryu, D.  and Tregillis, I. L. },
        citeulike-article-id = {2826460},
        doi = {10.1086/178151},
        eprint = {astro-ph/9606106},
        journal = {\apj},
        keywords = {1996, clumpyjet-paper},
        month = {December},
        pages = {365},
        posted-at = {2008-05-23 18:03:27},
        priority = {2},
        title = {The Magnetohydrodynamics of Supersonic Gas Clouds: MHD Cosmic Bullets and Wind-swept Clumps},
        url = {http://arxiv.org/abs/astro-ph/9606106},
        volume = {473},
        year = {1996}
}



@article{norman1979,
        abstract = {The paper considers the energy input to H2O masers in a dense molecular cloud and analyzes the response time scales for both collisional and radiative pump models. Specific mechanisms for magnetic energy input are given. The evolution of dense H2O maser clouds is studied in the environment of a young pre-main-sequence star that has developed an appreciable supersonic wind. It is shown that compact clouds can be ejected at high velocity to distances of order 1 pc. It is suggested that these clouds (referred to as interstellar bullets) might explain the phenomena of Herbig-Haro objects and high-velocity gas motions observed near compact infrared objects.},
        author = {Norman, C.  and Silk, J. },
        citeulike-article-id = {2821963},
        doi = {10.1086/156836},
        journal = {\apj},
        keywords = {1979, clumpyjet-paper},
        month = {February},
        pages = {197--205},
        posted-at = {2008-05-22 04:25:31},
        priority = {2},
        title = {Interstellar bullets - H2O masers and Herbig-Haro objects},
        url = {http://dx.doi.org/10.1086/156836},
        volume = {228},
        year = {1979}
}



@article{schwartz1978,
        abstract = {Detailed data on radial velocities and emission-line widths are presented for Herbig-Haro object No. 1 (HH 1) and seven of the condensations in HH 2. A theoretical model is proposed in which a strong stellar wind from an embedded pre-main-sequence star produces shock waves upon interaction with small ambient clouds, and radiating gas from bow shocks forms around dense cloudlets. A simple steady-state model of the stellar wind and its interaction with the interstellar medium is analyzed, and the physics of the interaction between the wind and a dense cloudlet is investigated. The ability of the proposed model to explain the salient observational features of HH objects is tested by comparison with the data obtained for HH 1 and HH 2. It is shown that the model provides plausible explanations for the low-excitation emission-line spectra, the radial velocities, the line widths, the total luminosity and variational time scale of a given condensation, and the lack of spatial coincidence between the nebular condensations and IR sources discovered near some HH objects. The model is less successful in accounting for the large velocity dispersion suggested by the line widths and the polarization observed in certain HH objects.},
        author = {Schwartz, R. D. },
        citeulike-article-id = {2821962},
        doi = {10.1086/156321},
        journal = {\apj},
        keywords = {1978, clumpyjet-paper},
        month = {August},
        pages = {884--887},
        posted-at = {2008-05-22 04:24:49},
        priority = {2},
        title = {A shocked cloudlet model for Herbig-Haro objects},
        url = {http://dx.doi.org/10.1086/156321},
        volume = {223},
        year = {1978}
}



@article{combet2008,
        abstract = {Context: The radial structure of accretion disks is a fundamental issue regarding star and planet formation. Many theoretical studies, focussing on different aspects such as e.g. disk emissivity or ionisation, have been conducted in the context of the standard accretion disk (SAD) model, where no jet is present. Aims: We wish to calculate the structure of young stellar object (YSO) accretion disks in an approach that takes into account the presence of the protostellar jets. The radial structure of these jet emitting disks (JED) should then be compared to that of SADs. Methods: The analytical treatment used in this work is similar to standard modelling of accretion disks but uses the parameter space of magnetised accretion-ejection structures that include the jet torque on the underlying disk. In this framework, the analytical expressions of key quantities are derived, such as mid-plane temperatures, surface densities or disk aspect ratios. Results: We find that JEDs present a structure different from the SADs, which can be observationally tested. The implications on planet formation in the inner regions of accretion disks are briefly discussed. We also supply sets of analytical formulae, valid in different opacity regimes, for the disk quantities. These expressions can be readily used for any work where the disk structure is needed as an input for the model.},
        author = {Combet, C.  and Ferreira, J. },
        citeulike-article-id = {2821030},
        doi = {10.1051/0004-6361:20078734},
        eprint = {0712.0913},
        journal = {\aap},
        keywords = {2008, clumpyjet-paper},
        month = {February},
        pages = {481--491},
        posted-at = {2008-05-21 19:42:48},
        priority = {2},
        title = {The radial structure of protostellar accretion disks: influence of jets},
        url = {http://arxiv.org/abs/0712.0913},
        volume = {479},
        year = {2008}
}



@article{konigl1982,
        abstract = {An attempt is made to present a unified interpretation of anisotropic emission and outflow phenomena which are detected over a wide range of scales in the vicinity of young stellar objects embedded in dense molecular clouds. The evolution of an interstellar bubble in an anisotropic medium is considered, and the formation and propagation of jets, and their relation to the various bipolar phenomena observed in molecular clouds, are discussed. The possible role of magnetic fields in reproducing bipolar emission sources is examined. It is found that an isotropic stellar wind which expands in a medium with an anisotropic density distribution would give rise to an interstellar bubble which elongates in the direction of the external density gradient. Under certain conditions which are likely to prevail in protostellar environments, the elongating bubble could become unstable to the formation of de Laval nozzles. Once these are established, the outflow becomes channeled into two oppositely directed, supersonic jets.},
        author = {K\"onigl, A. },
        citeulike-article-id = {2820991},
        doi = {10.1086/160324},
        journal = {\apj},
        keywords = {1982, clumpyjet-paper},
        month = {October},
        pages = {115--134},
        posted-at = {2008-05-21 19:22:26},
        priority = {2},
        title = {On the nature of bipolar sources in dense molecular clouds},
        url = {http://dx.doi.org/10.1086/160324},
        volume = {261},
        year = {1982}
}



@article{reipurth1988hh58:82,
        abstract = {A list of 25 new Herbig-Haro objects, HH 58 to HH 82, in the Orion molecular clouds and in southern molecular cloud complexes has been compiled. CCD images in the S II 6717, 6731 forbidden lines are presented for the objects, together with a few spectra and some IR observations. The individual objects and, when identified, their energy sources are discussed. HH 65 is located in the red lobe of the bipolar outflow associated with the highly variable reflection nebula Re 50. HH 67 is a 22-arcsec long sinusoidal jet. HH 68/69 consists of a long, linear chain of four HH knots. HH 72 emerges from a 120-solar luminosity IRAS source embedded in a Bok globule. HH 79 is the first HH object discovered in the Ophiuchus clouds. HH 80/81 in Sagittarius are among the brightest HH objects known, have complex velocities, high excitation conditions and emerge from a 6000-solar luminosity young B-star. HH 82 is associated with the bright variable star S Coronae Australis.},
        author = {Reipurth, B. and Graham, J. A. },
        citeulike-article-id = {2817220},
        journal = {\aap},
        keywords = {1988, hh-58, hh-82},
        pages = {219--239},
        posted-at = {2008-05-20 18:12:28},
        priority = {2},
        title = {New Herbig-Haro objects in star-forming regions},
        url = {http://adsabs.harvard.edu/abs/1988A\%26A...202..219R},
        volume = {202},
        year = {1988}
}



@article{mundt1983hh30,
        abstract = {The discovery of four jetlike emission-line nebulosities associated with DG Tau, DG Tau B, HH 30, and HL Tau, and the confirmation of the IRS 5 jet in L1551 are reported. All these jets have typical lengths of 2-4 x 10 to the 16th cm and small opening angles of 5 deg-10 deg. The observations strongly suggest that these jets are due to a highly collimated mass outflow. Their collimation must take place at distances smaller than 3 x 10 to the 15th cm from the jet sources. Many CO outflows observed near low to medium luminosity sources (0.1-100 solar luminosities) may be driven by jets, similar to the newly discovered ones.},
        author = {Mundt, R.  and Fried, J. W. },
        citeulike-article-id = {2817141},
        doi = {10.1086/184155},
        journal = {\apjl},
        keywords = {1983, hh-30},
        month = {November},
        pages = {L83--L86},
        posted-at = {2008-05-20 17:24:15},
        priority = {2},
        title = {Jets from young stars},
        url = {http://dx.doi.org/10.1086/184155},
        volume = {274},
        year = {1983}
}



@article{smith1997,
        abstract = {The jet model for protostellar outflows is confronted with the constraints imposed by CO spectroscopic observations. From three dimensional simulations of a dense molecular medium being penetrated by a denser molecular jet, we simulate line profiles and construct position-velocity diagrams for the (low-J) CO transitions. We find (1) the profiles imply power law variation of integrated brightness with velocity over a wide range of velocities, (2) the velocity field resembles a `Hubble Law' and (3) a hollow-shell structure at low velocities becomes an elongated lobe at high velocities. Moreover, the leading bow shock produces strong forward motion of the cool gas rather than the expected lateral expansion. We are thus able to satisfy the Lada and Fich (1996ApJ...459..638L) criteria, employing NGC 2264G as an example. Deviations from the simple power law dependence of integrated brightness versus velocity occur at high velocities in our simulations. The curve first dips to a shallow minimum and then rises rapidly and peaks sharply. Reanalysis of the NGC 2264G and Cepheus E data confirm these predictions. We identify these two features with a jet-ambient shear layer and the jet itself. A deeper analysis reveals that the power-law index is an indicator of the evolutionary stage: a profile steepens with time. Also, the CO excitation temperature changes along the bow walls and thus a CO line intensity does not directly yield the mass distribution, as often assumed. Instead, the CO emission is enhanced near the excitation peaks.},
        author = {Smith, M. D.  and Suttner, G.  and Yorke, H. W. },
        citeulike-article-id = {2814330},
        journal = {\aap},
        keywords = {1997},
        pages = {223--230},
        posted-at = {2008-05-19 22:47:04},
        priority = {2},
        title = {Numerical hydrodynamic simulations of jet-driven bipolar outflows.},
        volume = {323},
        year = {1997}
}



@article{schwartz1975hh155,
        abstract = {Radial velocities of the emission nebulae and NGC 1555 (Hind's Reflection Nebula) which are associated with T Tau suggest the presence of extended mass outflow which is supersonic with respect to the medium in which the star is embedded. It is suggested that radiating shocks may form where the flow interfaces with the intracloud medium, producing emission spectra similar to that predicted by the shock-wave models of Cox. An electron density and temperature analysis based upon the relative intensities of the near-infrared and blue lines of forbidden O II in Burnham's Emission Nebula supports the shock wave hypothesis. The character of the emission-line spectrum, the small filling factor, and the energy balance requirements of the system are also compatible with the hypothesis. The Herbig-Haro Nebulae, if produced by the same mechanism, must involve central objects with a considerably higher rate of mass outflow than is indicated for T Tau.},
        author = {Schwartz, R. D. },
        citeulike-article-id = {2814018},
        journal = {\apj},
        keywords = {1975, hh-155},
        month = {February},
        pages = {631--642},
        posted-at = {2008-05-19 20:49:48},
        priority = {2},
        title = {T Tauri Nebulae and Herbig-Haro Nebulae - Evidence for excitation by a strong stellar wind},
        url = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1975ApJ...195..631S},
        volume = {195},
        year = {1975}
}



@article{reipurth1991hh110,
        abstract = {The L1617 cloud in the Orion B complex at optical, infrared, and millimeter wavelengths have been studied, and a number of regions containing Herbig-Haro objects, molecular outflows, nebulous stars, and infrared sources have been found, testifying to very recent star formation events. HH 110 is a spectacular, more than 3 arcmin long winding jet with numerous knots embedded in a matrix of low-luminosity gas. HH 111, a highly collimated jet with several bow shocks in a bipolar complex, is associated with a major molecular outflow; the energy source is embedded in a 30 solar mass cloud core. HH 112 is a very faint chain of emission line knots, and HH 113 is a complex group of knots with a jet. The embedded source IRAS 04587+0255, unrelated to any of the HH objects, is driving a large bipolar molecular outflow; the source is located in a region of dense gas containing several other embedded sources.},
        author = {Reipurth, B. and Olberg, M. },
        citeulike-article-id = {2813865},
        journal = {\aap},
        keywords = {1991, hh-110},
        pages = {535--550},
        posted-at = {2008-05-19 19:35:16},
        priority = {2},
        title = {Herbig-Haro jets and molecular outflows in L1617},
        volume = {246},
        year = {1991}
}



@article{reipurth2001ar,
        abstract = {Abstract Outflow activity is associated with all stages of early stellar evolution, from deeply embedded protostellar objects to visible young stars. Herbig-Haro (HH) objects are the optical manifestations of this powerful mass loss. Analysis of HH flows, and in particular of the subset of highly collimated HH jets, provides indirect but important insights into the nature of the accretion and mass-loss processes that govern the formation of stars. The recent recognition that HH flows may attain parsec-scale dimensions opens up the possibility of partially reconstructing the mass-ejection history of the newly born driving sources and, therefore, their mass-accretion history. Furthermore, HH flows are astrophysical laboratories for the analysis of shock structures, of hydrodynamics in collimated flows, and of their interaction with the surrounding environment. HH flows may be an important source of turbulence in molecular clouds. Recent technological developments have enabled detailed observations of outflows from young stars at near-infrared, mid-infrared, submillimeter, millimeter, and centimeter wavelengths, providing a comprehensive picture of the outflow phenomenon of young stars.},
        author = {Reipurth, B. and Bally, J. },
        citeulike-article-id = {2813842},
        doi = {10.1146/annurev.astro.39.1.403},
        journal = {\araa},
        keywords = {2001, annual-review},
        number = {1},
        pages = {403--455},
        posted-at = {2008-05-19 19:26:16},
        priority = {2},
        title = {HERBIG-HARO FLOWS: Probes of Early Stellar Evolution},
        url = {http://arjournals.annualreviews.org/doi/abs/10.1146/annurev.astro.39.1.403},
        volume = {39},
        year = {2001}
}



@article{bachiller1996ar,
        abstract = {Abstract A violent outflow of high-velocity gas is one of the first manifestations of the formation of a new star. Such outflows emerge bipolarly from the young object and involve amounts of energy similar to those involved in accretion processes. The youngest (proto-)stellar low-mass objects known to date (the Class 0 protostars) present a particularly efficient outflow activity, indicating that outflow and infall motions happen simultaneously and are closely linked since the very first stages of the star formation processes. This article reviews the wealth of information being provided by large millimeter-wave telescopes and interferometers on the small-scale structure of molecular outflows, as well as the most recent theories about their origin. The observations of highly collimated CO outflows, extremely high velocity (EHV) flows, and molecular bullets are examined in detail, since they provide key information on the origin and propagation of outflows. The peculiar chemistry operating in the associated shocked molecular regions is discussed, highlighting the recent high-sensitivity observations of low-luminosity sources. The classification schemes and the properties of the driving sources of bipolar outflows are summarized with special attention devoted to the recently identified Class 0 protostars. All these issues are crucial for building a unified theory on the mass-loss phenomena in young stars.},
        author = {Bachiller, R.  },
        citeulike-article-id = {2813831},
        doi = {10.1146/annurev.astro.34.1.111},
        journal = {\araa},
        keywords = {1996, annual-review},
        number = {1},
        pages = {111--154},
        posted-at = {2008-05-19 19:23:21},
        priority = {2},
        title = {BIPOLAR MOLECULAR OUTFLOWS FROM YOUNG STARS AND PROTOSTARS},
        url = {http://arjournals.annualreviews.org/doi/abs/10.1146/annurev.astro.34.1.111},
        volume = {34},
        year = {1996}
}



@article{schwartz1983ar,
        author = {Schwartz, R. D. },
        citeulike-article-id = {2813823},
        doi = {10.1146/annurev.aa.21.090183.001233},
        journal = {\araa},
        keywords = {1983, annual-review},
        number = {1},
        pages = {209--237},
        posted-at = {2008-05-19 19:19:14},
        priority = {2},
        title = {Herbig-Haro Objects},
        url = {http://arjournals.annualreviews.org/doi/abs/10.1146/annurev.aa.21.090183.001233},
        volume = {21},
        year = {1983}
}



@article{haro1952,
        abstract = {Not Available},
        author = {Haro, G. },
        citeulike-article-id = {2813644},
        doi = {10.1086/145576},
        journal = {\apj},
        keywords = {1952, hh-1, hh-2},
        month = {May},
        pages = {572--573},
        posted-at = {2008-05-19 17:50:33},
        priority = {2},
        title = {Herbig's Nebulous Objects Near NGC 1999.},
        url = {http://dx.doi.org/10.1086/145576},
        volume = {115},
        year = {1952}
}



@article{herbig1951,
        abstract = {Not Available},
        author = {Herbig, G. H. },
        citeulike-article-id = {2813642},
        doi = {10.1086/145440},
        journal = {\apj},
        keywords = {1951, hh-1, hh-2},
        month = {May},
        pages = {697--699},
        posted-at = {2008-05-19 17:49:58},
        priority = {2},
        title = {The Spectra of Two Nebulous Objects Near NGC 1999.},
        url = {http://dx.doi.org/10.1086/145440},
        volume = {113},
        year = {1951}
}


@ARTICLE{ostriker2001,
   author = {{Ostriker}, E.~C. and {Lee}, {C.-F.} and {Stone}, J.~M. and 
        {Mundy}, L.~G.},
    title = "{A Ballistic Bow Shock Model for Jet-driven Protostellar Outflow Shells}",
  journal = {\apj},
   eprint = {arXiv:astro-ph/0104374},
 keywords = {Hydrodynamics, ISM: Jets and Outflows, Methods: Analytical, Stars: Formation},
     year = 2001,
    month = aug,
   volume = 557,
    pages = {443-450},
      doi = {10.1086/321649},
   adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...557..443O},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}





@article{ostriker2001molecularclouds,
        author = {Ostriker, Eve  C.  and Stone, James  M.  and Gammie, Charles  F. },
        citeulike-article-id = {2808368},
        journal = {\apj},
        keywords = {2001, clumpyjet-paper},
        month = {January},
        pages = {980--1005},
        posted-at = {2008-05-18 00:05:51},
        priority = {2},
        title = {Density, Velocity, and Magnetic Field Structure in Turbulent Molecular Cloud Models},
        url = {http://adsabs.harvard.edu/cgi-bin/bib\_query?2001ApJ...546..980O},
        volume = {546},
        year = {2001}
}



@article{reipurth2002hh34,
        abstract = {We present new, deep Halpha and [S II] images of the HH 34 jet and bow shock obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST), which reveal the structure of this fine HH flow with unprecedented detail. Many of the knots in the jet appear to form small working surfaces with bright [S II] cores and thin Halpha filaments where the mini-bow shocks extend into the surrounding medium. In combination with earlier, short-exposure HST images we have determined very precise proper-motion vectors for the various shock structures in the outflow. The jet becomes visible within about an arcsecond of the source, where a new knot has emerged between our two epoch images; it has a space velocity of at least 300 km s<SUP>-1</SUP>, as derived from the proper motions and correcting for the 30° angle of the flow to the line of sight. The jet rapidly slows down to a mean space velocity of about 220 km s<SUP>-1</SUP>, with a standard deviation of 20 km s<SUP>-1</SUP> among the jet knots. Such low internal velocities lead to weak shocks, consistent with the high [S II]/Halpha ratio along the jet body and in accordance with the internal working surface model for jets. The jet motion appears to be ballistic, with no evidence for a turbulent boundary layer. The jet is well resolved and steadily expands with a half-opening angle of 0.4d. The large HH 34 working surface shows a multitude of knots, all of which are enveloped by a series of very thin, limb-brightened Halpha-emitting filaments immediately behind the shock front where the flow faces into the preshock medium. One of these filaments developed four regularly spaced tiny knots between the two epochs, possibly due to a Rayleigh-Taylor instability along the filament or caused by the presence of small, dense clumps in the ambient medium. Proper motions of the HH 34 working surface show an obvious expansion due to material being squirted sideways. In addition to the large-scale S-shaped symmetry of the giant HH 34 flow, the jet shows a marked and surprisingly abrupt change in flow direction during a 65 yr interval that ended 10 yr ago, suggesting that the jet-disk system may have been influenced by powerful tidal effects by a companion star during a recent periastron passage. A second, smaller bowlike flow, called HH 534, possibly emanates from the HH 34 source region, and if so this supports the contention that the source is a binary. This data set is a testament to the unique abilities of the HST to follow morphological, photometric, and excitation changes on cooling timescales in the shocks of flows from young stars.},
        author = {Reipurth, B.  and Heathcote, S.  and Morse, J.  and Hartigan, P.  and Bally, J. },
        citeulike-article-id = {2808360},
        doi = {10.1086/324738},
        journal = {\aj},
        keywords = {2002, clumpyjet-paper},
        month = {January},
        pages = {362--381},
        posted-at = {2008-05-17 23:55:13},
        priority = {2},
        title = {Hubble Space Telescope Images of the HH 34 Jet and Bow Shock: Structure and Proper Motions},
        url = {http://dx.doi.org/10.1086/324738},
        volume = {123},
        year = {2002}
}



@article{hartigan2005hh47,
        abstract = {We present a proper-motion study of the shock waves within the classic stellar jet HH 47 based on Hubble Space Telescope (HST) Halpha and [S II] images of the region taken over two epochs. Individual knots within the jet and in the bow shock/Mach disk working surface of HH 47A move significantly in the 5 yr that separate the images, and the excellent spatial resolution of HST makes it possible to measure the proper motions with enough precision to easily observe differential motions throughout the flow. The bright portion of the jet emerges at 37.5d+/-2.5d from the plane of the sky with an average velocity of 300 km s<SUP>-1</SUP>. Dynamical ages of the shock waves in the jet range from a few decades for knots recently ejected by the source to ~1300 yr for the faint extended bow shock HH 47D. The jet curves, but motions of knots in the jet are directed radially away from the exciting source, and velocity variability in the flow drives the shock waves that heat the jet internally. The jet orientation angle varies with time by about 15° and currently points to the northwestern portion of a cavity outlined by a reflection nebula, where a quasi-stationary shock deflects the jet. The major working surface HH 47A is more complex than a simple bow shock/Mach disk and contains numerous clumps that move relative to one another with velocities of ~+/-40 km s<SUP>-1</SUP>. Small clumps or instabilities affect the Mach disk, and dense clumps may move all the way through the working surface to cause the bumpy morphology seen at the bow shock. A localized area between the bow shock and Mach disk varies significantly between the two sets of images.<p> Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.},
        author = {Hartigan, P.  and Heathcote, S.  and Morse, J. A.  and Reipurth, B.  and Bally, J. },
        citeulike-article-id = {2808353},
        doi = {10.1086/491673},
        eprint = {astro-ph/0507526},
        journal = {\aj},
        keywords = {2005, clumpyjet-paper},
        month = {November},
        pages = {2197--2205},
        posted-at = {2008-05-17 23:41:23},
        priority = {2},
        title = {Proper Motions of the HH 47 Jet Observed with the Hubble Space Telescope},
        url = {http://arxiv.org/abs/astro-ph/0507526},
        volume = {130},
        year = {2005}
}

@INPROCEEDINGS{raga2003,
   author = {{Raga}, A.~C. and {Vel{\'a}zquez}, P.~F. and {de Gouveia dal Pino}, E.~M. and 
        {Noriega-Crespo}, A. and {Mininni}, P.},
    title = "{Entrainment in Herbig-Haro Objects}",
 keywords = {ISM: Jets and outflows, Stars: Mass loss, Stars: Pre-main sequence},
booktitle = {Revista Mexicana de Astronomia y Astrofisica Conference Series},
     year = 2003,
   series = {Revista Mexicana de Astronomia y Astrofisica Conference Series},
   volume = 15,
   editor = "{J.~Arthur \& W.~J.~Henney}",
    month = jan,
    pages = {115-119},
   adsurl = {http://adsabs.harvard.edu/abs/2003RMxAC..15..115R},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@article{raga2002hh110,
        abstract = {We present 3D, gasdynamic simulations of jet/cloud collisions, with the purpose of modelling the HH 270/110 system. From the models, we obtain predictions of Halpha and H\_2 1-0 s(1) emission line maps, which qualitatively reproduce some of the main features of the corresponding observations of HH 110. We find that the model that better reproduces the observed structures corresponds to a jet that was deflected at the surface of the cloud ~ 1000 yr ago, but is now boring a tunnel directly into the cloud. This model removes the apparent contradiction between the jet/cloud collision model and the lack of detection of molecular emission in the crossing region of the HH 270 and HH 110 axes.},
        author = {Raga, A. C.  and de Gouveia Dal Pino, E. M. and Noriega-Crespo, A.  and Mininni, P. D.  and Vel\'{a}zquez, P. F. },
        citeulike-article-id = {2808350},
        doi = {10.1051/0004-6361:20020851},
        eprint = {astro-ph/0206242},
        journal = {\aap},
        keywords = {2002, clumpyjet-paper},
        month = {September},
        pages = {267--276},
        posted-at = {2008-05-17 23:37:24},
        priority = {2},
        title = {Jet/cloud collision, 3D gasdynamic simulations of HH 110},
        url = {http://arxiv.org/abs/astro-ph/0206242},
        volume = {392},
        year = {2002}
}



@article{raga1993,
        abstract = {<img src="http://adsabs.harvard.edu/articles/abstracts/1993/MNRAS/1993MNRAS.264..758R.gif"><p>},
        author = {Raga, A. C.  and Biro, S. },
        citeulike-article-id = {2808346},
        journal = {\mnras},
        keywords = {1993, clumpyjet-paper},
        month = {October},
        pages = {758},
        posted-at = {2008-05-17 23:35:23},
        priority = {2},
        title = {Machine-Gun Jets from Time-Dependent Sources},
        url = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1993MNRAS.264..758R},
        volume = {264},
        year = {1993}
}



@article{biro1994,
        abstract = {A numerical simulation of a stellar jet with a supersonic variation in the magnitude of the outflow velocity is presented. The structure, evolution, and the observational properties of this model are studied. A qualitative comparison is made both with previous analytic predictions and with observations of Herbig-Haro jets.},
        author = {Biro, S.  and Raga, A. C. },
        citeulike-article-id = {2808345},
        doi = {10.1086/174719},
        journal = {\apj},
        keywords = {1994, clumpyjet-paper},
        month = {October},
        pages = {221--231},
        posted-at = {2008-05-17 23:35:01},
        priority = {2},
        title = {A numerical simulation of a variable velocity jet},
        url = {http://dx.doi.org/10.1086/174719},
        volume = {434},
        year = {1994}
}



@article{suttner1997,
        author = {Suttner, G.  and Smith, M. D.  and Yorke, H. W.  and Zinnecker, H. },
        citeulike-article-id = {2808343},
        journal = {\aap},
        keywords = {1997, clumpyjet-paper},
        pages = {595--607},
        posted-at = {2008-05-17 23:31:56},
        priority = {2},
        title = {Multi-dimensional numerical simulations of molecular jets.},
        volume = {318},
        year = {1997}
}



@article{raga1990ws,
        abstract = {Models for high Mach number, isothermal, pressure-matched jets ejected from sources with variable velocities are presented. It is found that the relaxation of the assumption of a time-independent source allows the complex position-velocity diagrams and multiple bow shock structures observed in some stellar jets to be explained in a straightforward way. Analytic and numerical models are presented for jets with variable velocity sources. A comparison with previously published observations of the HH 46/47 jet is performed which shows how the velocity variations observed along a jet can be used to reconstruct the past time variability of the source. This technique is promising for future studies of the mechanism by which stellar jets are produced.},
        author = {Raga, A. C.  and Binette, L.  and Canto, J.  and Calvet, N. },
        citeulike-article-id = {2808329},
        doi = {10.1086/169443},
        journal = {\apj},
        keywords = {1990, clumpyjet-paper},
        month = {December},
        pages = {601--610},
        posted-at = {2008-05-17 23:18:32},
        priority = {2},
        title = {Stellar jets with intrinsically variable sources},
        url = {http://dx.doi.org/10.1086/169443},
        volume = {364},
        year = {1990}
}



@article{raga1990internal,
        abstract = {Models of nonadiabatic, high Mach number, cylindrically symmetric, steady stellar jets have been computed. In these calculations, the effects of the nonequilibrium ionization and cooling have been taken into consideration. An extensive study of parameter space (limited to initially overpressured jets) provides a qualitative picture of the different characteristics possible for stellar jets. In particular, it is found that, for parameters typical of stellar jets, the internal jet shocks produce only a low degree of ionization. This result qualitatively agrees with observations of stellar jets, which typically show a low excitation spectrum.},
        author = {Raga, A. C.  and Binette, L.  and Canto, J. },
        citeulike-article-id = {2808326},
        doi = {10.1086/169149},
        journal = {\apj},
        keywords = {1990, clumpyjet-paper},
        month = {September},
        pages = {612--625},
        posted-at = {2008-05-17 23:18:13},
        priority = {2},
        title = {Steady, partially ionized stellar jets},
        url = {http://dx.doi.org/10.1086/169149},
        volume = {360},
        year = {1990}
}



@article{buehrke1988,
        author = {B\"uhrke, T.  and Mundt, R.  and Ray, T. P. },
        citeulike-article-id = {2808323},
        journal = {\aap},
        keywords = {1988, clumpyjet-paper},
        pages = {99--119},
        posted-at = {2008-05-17 23:14:53},
        priority = {2},
        title = {A detailed study of HH 34 and its associated jet},
        volume = {200},
        year = {1988}
}



@article{rees1978,
        abstract = {If the M87 radio source is energized by plasma beams collimated in the nucleus, then the optical 'knots' in the jet can be interpreted as internal shocks which develop from velocity irregularities in the beam. The optical continuum in the 'knots' is synchrotron emission from short-lived electrons accelerated by such shocks; lower energy electrons, with longer lifetimes, escape sideways to provide an energy input into the radio components. The fact that the optical jet is asymmetric with respect to the nucleus, despite the symmetry of the overall radio structure, implies either some difference between the beams, or relativistic speeds. In the latter case, the central 'nozzles' would have to vary on a characteristic time-scale of a few hundred years.},
        author = {Rees, M. J. },
        citeulike-article-id = {2808321},
        journal = {\mnras},
        keywords = {1978, clumpyjet-paper},
        month = {September},
        pages = {61P--65P},
        posted-at = {2008-05-17 23:10:23},
        priority = {2},
        title = {The M87 jet - Internal shocks in a plasma beam},
        url = {http://adsabs.harvard.edu/cgi-bin/nph-bib\_query?bibcode=1978MNRAS.184P..61R},
        volume = {184},
        year = {1978}
}



@unpublished{dennis2008windclump,
        author = {Dennis, T.  and Frank, A.  and Blackman, E.  and Yirak, K. },
        booktitle = {in preparation},
        citeulike-article-id = {2805735},
        keywords = {clumpyjet-paper},
        posted-at = {2008-05-16 20:13:10},
        priority = {2},
        title = {Untitled},
        year = {In preparation}
}



@article{velusamy2007hh46/47,
        abstract = {We present new details of the structure and morphology of the jets and outflows in HH 46/47 as seen in Spitzer infrared images from IRAC and MIPS, reprocessed using the “HiRes” deconvolution technique. HiRes improves the visualization of spatial morphology by enhancing resolution (to subarcsecond levels in IRAC bands) and removing the contaminating side lobes from bright sources. In addition to sharper views of previously reported bow shocks, we have detected (1) the sharply delineated cavity walls of the wide-angle biconical outflow, seen in scattered light on both sides of the protostar, (2) several very narrow jet features at distances ~400 AU to ~0.1 pc from the star, and (3) compact emissions at MIPS 24 mum coincident with the jet heads, tracing the hottest atomic/ionic gas in the bow shocks. Together the IRAC and MIPS images provide a more complete picture of the bow shocks, tracing both the molecular and atomic/ionic gases, respectively. The narrow width and alignment of all jet-related features indicate a high degree of jet collimation and low divergence (width of ~400 AU increasing by only a factor of 2.3 over 0.2 pc). The morphology of this jet, bow shocks, wide-angle outflows, and the fact that the jet is nonprecessing and episodic, constrain the mechanisms for producing the jet's entrained molecular gas, and origins of the fast jet, and slower wide-angle outflow.},
        author = {Velusamy, T.  and Langer, W. D.  and Marsh, K. A. },
        citeulike-article-id = {2805728},
        doi = {10.1086/522929},
        eprint = {0710.0597},
        journal = {\apjl},
        keywords = {2007, clumpyjet-paper},
        month = {October},
        pages = {L159--L162},
        posted-at = {2008-05-16 20:07:50},
        priority = {2},
        title = {Highly Collimated Jets and Wide-Angle Outflows in HH 46/47: New Evidence from Spitzer Infrared Images},
        url = {http://arxiv.org/abs/0710.0597},
        volume = {668},
        year = {2007}
}



@article{raga1998hh34,
        abstract = {Variable ejection velocity jet models can qualitatively explain the appearance of successive working surfaces in Herbig-Haro (HH) jets. This paper presents an attempt to explore which features of the HH 34 jet can indeed be reproduced by such a model. From previously published data on this object, we find evidence for the existence of a three-mode ejection velocity variability and then explore the implications of such a variability. From simple, analytic considerations it is possible to show that the longer period modes produce a modulation of the shorter period modes, resulting in the formation of “trains” of multiple knots. The knots observed close to the source of HH 34 could correspond to such a structure. Finally, a numerical simulation with the ejection velocity variability deduced from the HH 34 data is computed. This numerical simulation shows a quite remarkable resemblance with the observed properties of the HH 34 jet.},
        author = {Raga, A.  and Noriega-Crespo, A. },
        citeulike-article-id = {2805621},
        doi = {10.1086/300641},
        eprint = {astro-ph/9808280},
        journal = {\aj},
        keywords = {1998, clumpyjet-paper},
        month = {December},
        pages = {2943--2952},
        posted-at = {2008-05-16 18:40:16},
        priority = {2},
        title = {A Three-mode, Variable Velocity Jet Model for HH 34},
        url = {http://arxiv.org/abs/astro-ph/9808280},
        volume = {116},
        year = {1998}
}



@article{dalgarno1972,
        author = {Dalgarno, A.  and McCray, R. A. },
        citeulike-article-id = {2805618},
        journal = {\araa},
        keywords = {1972, clumpyjet-paper},
        pages = {375--426},
        posted-at = {2008-05-16 18:37:35},
        priority = {2},
        title = {Heating and Ionization of HI Regions},
        volume = {10},
        year = {1972}
}



@article{volker1999,
        abstract = {Very young protostars eject collimated jets of molecular gas. Although the protostars themselves are hidden, some of their properties are revealed through the jet dynamics. We here model velocity shear, precession, pulsation and spray within dense jets injected into less-dense molecular clouds. We investigate the Hammer Jet, for which extreme velocity variations as well as strong ripping and spray actions are introduced. A three dimensional ZEUS-type hydrodynamics code, extended with molecular physics, is employed.

Jet knots, previously shown to be compact in simulations of smoother jets, now appear as prominent bow shocks in H2 and as bullets in CO emission lines. High proper motions are predicted in the jet. In the lobes we uncover wide tubular low-velocity CO structures with concave bases near the nozzle. Proper motion vectors in the lobes delineate a strong accelerated flow away from the head with some superimposed turbulent-like motions. The leading bow is gradually distorted by the hammer blows and breaks up into mini-bow segments. The H2 emission line profiles are wide and twin-peaked over much of the leading bow.

On comparison with the simulations, we identify observed outflows driven by various dynamical types of jet. Shear is essential to produce the jet bows, spray or precession to widen the outflows and hammer blows to generate knotty jets. We identify the proper motions of maser spots with the pattern speed of density peaks in the inner jet and shell.},
        author = {V\"olker, Roland   and Smith, Michael  D.  and Suttner, Gerhard   and Yorke, Harold  W. },
        citeulike-article-id = {2805603},
        journal = {\aap},
        keywords = {1999, clumpyjet-paper},
        month = {March},
        pages = {953--965},
        posted-at = {2008-05-16 18:25:06},
        priority = {0},
        title = {Numerical hydrodynamic simulations of molecular outflows driven by Hammer jets},
        url = {http://aa.springer.de/bibs/9343003/2300953/small.htm},
        volume = {343},
        year = {1999}
}



@article{hartigan2007bfields,
        abstract = {Although several lines of evidence suggest that jets from young stars are driven magnetically from accretion disks, existing observations of field strengths in the bow shocks of these flows imply that magnetic fields play only a minor role in the dynamics at these locations. To investigate this apparent discrepancy we performed numerical simulations of expanding magnetized jets with stochastically variable input velocities with the AstroBEAR MHD code. Because the magnetic field B is proportional to the density n within compression and rarefaction regions, the magnetic signal speed drops in rarefactions and increases in the compressed areas of velocity-variable flows. In contrast, B~n<SUP>0.5</SUP> for a steady state conical flow with a toroidal field, so the Alfv\'{e}n speed in that case is constant along the entire jet. The simulations show that the combined effects of shocks, rarefactions, and divergent flow cause magnetic fields to scale with density as an intermediate power 1>p>0.5. Because p>0.5, the Alfv\'{e}n speed in rarefactions decreases on average as the jet propagates away from the star. Hence, a typical Alfv\'{e}n velocity in the jet close to the star is significantly larger than it is in the rarefactions ahead of bow shocks at larger distances. We find that the observed values of weak fields at large distances are consistent with strong fields required to drive the observed mass loss close to the star. Typical velocity perturbations, which form shocks at large distances, will produce only magnetic waves close to the star. For a typical stellar jet the crossover point inside which velocity perturbations of 30-40 km s<SUP>-1</SUP> no longer produce shocks is ~300 AU from the source.},
        author = {Hartigan, P.  and Frank, A.  and Varni\'{e}re, P.  and Blackman, E. G. },
        citeulike-article-id = {2802583},
        doi = {10.1086/513499},
        eprint = {astro-ph/0702174},
        journal = {\apj},
        keywords = {2007, clumpyjet-paper},
        month = {June},
        pages = {910--918},
        posted-at = {2008-05-15 20:50:45},
        priority = {2},
        title = {Magnetic Fields in Stellar Jets},
        url = {http://arxiv.org/abs/astro-ph/0702174},
        volume = {661},
        year = {2007}
}



@article{heathcote1996hubble,
        abstract = {Not Available},
        author = {Heathcote, S.  and Morse, J. A.  and Hartigan, P.  and Reipurth, B.  and Schwartz, R. D.  and Bally, J.  and Stone, J. M. },
        citeulike-article-id = {2802582},
        doi = {10.1086/118085},
        journal = {\aj},
        keywords = {1996, clumpyjet-paper},
        month = {September},
        pages = {1141--1168},
        posted-at = {2008-05-15 20:49:51},
        priority = {2},
        title = {Hubble Space Telescope Observations of the HH 47 Jet: Narrowband Images},
        url = {http://dx.doi.org/10.1086/118085},
        volume = {112},
        year = {1996}
}



@article{micono1998khjets,
        abstract = {We discuss the spatial evolution into biconical shocks of axisymmetric perturbations in supersonic jets subject to non-equilibrium radiative losses. Our aim is to interpret the origin of the knots, observed along many jets in Young Stellar Objects (YSOs), in terms of shocks originated by Kelvin-Helmholtz modes. In this scheme, we find that the \$[SII]/H\_α\$ line intensity ratios and the mean intra-knot spacing result connected to each other, and we show the evolution of the shock morphologies as a consequence of shock merging effects. From the numerical calculations we also obtain the knot proper motion velocities and the line flux behavior along the jet and make comparisons with the observations.},
        author = {Micono, M.  and Massaglia, S.  and Bodo, G.  and Rossi, P.  and Ferrari, A. },
        citeulike-article-id = {2802569},
        journal = {\aap},
        keywords = {1998, clumpyjet-paper},
        pages = {1001--1006},
        posted-at = {2008-05-15 20:41:43},
        priority = {2},
        title = {Kelvin-Helmholtz instabilities in stellar jets. IV. On the origin of the emission knots},
        volume = {333},
        year = {1998}
}



@article{xu2000jetstability3d,
        abstract = {The effect of optically thin radiative cooling on the Kelvin-Helmholtz instability of three-dimensional jets is investigated via linear stability theory and nonlinear hydrodynamical simulation. Two different cooling functions are considered; radiative cooling is found to have a significant effect on the stability of the jet in each case. The wavelengths and growth rates of unstable modes in the numerical simulations are found to be in good agreement with theoretical predictions. Disruption of the jet is found to be sensitive to the precessional frequency at the origin, with lower frequencies leading to more rapid disruption. Strong nonlinear effects are observed as the result of the large number of normal modes in three dimensions which provide rich mode-mode interactions. These mode-mode interactions provide new mechanisms for the formation of knots in the flows. Significant structural features found in the numerical simulations appear similar to structures observed on protostellar jets.},
        author = {Xu, J.  and Hardee, P. E.  and Stone, J. M. },
        citeulike-article-id = {2802558},
        doi = {10.1086/317094},
        eprint = {astro-ph/0007446},
        journal = {\apj},
        keywords = {2000, clumpyjet-paper},
        month = {November},
        pages = {161--177},
        posted-at = {2008-05-15 20:35:33},
        priority = {2},
        title = {The Stability of Radiatively Cooled Jets in Three Dimensions},
        url = {http://arxiv.org/abs/astro-ph/0007446},
        volume = {543},
        year = {2000}
}



@article{ouyed2003jetstability,
        abstract = {We present the extension of previous two-dimensional simulations of the time-dependent evolution of nonrelativistic outflows from the surface of Keplerian accretion disks to three dimensions. As in the previous work, we investigate the outflow that arises from a magnetized accretion disk that is initially in hydrostatic balance with its surrounding cold corona. The accretion disk itself is taken to provide a set of fixed boundary conditions for the problem. We find that the mechanism of jet acceleration is identical to what was established from the previous two-dimensional simulations. The three-dimensional results are consistent with the theory of steady, axisymmetric, centrifugally driven disk winds up to the Alfv\'{e}n surface of the outflow. Beyond the Alfv\'{e}n surface, however, the jet in three dimensions becomes unstable to nonaxisymmetric, Kelvin-Helmholtz instabilities. The most important result of our work is that while the jet is unstable at super-Alfv\'{e}nic speeds, it survives the onset of unstable modes that appear in this physical regime. We show that jets maintain their long-term stability through a self-limiting process wherein the average Alfv\'{e}nic Mach number within the jet is maintained to the order of unity. This is accomplished in at least two ways. First, the poloidal magnetic field is concentrated along the central axis of the jet forming a “backbone” in which the Alfv\'{e}n speed is sufficiently high to reduce the average jet Alfv\'{e}nic Mach number to unity. Second, the onset of higher order Kelvin-Helmholtz “flute” modes (m>=2) reduces the efficiency with which the jet material is accelerated and transfers kinetic energy of the outflow into the stretched, poloidal field lines of the distorted jet. This too has the effect of increasing the Alfv\'{e}n speed and thereby reducing the Alfv\'{e}nic Mach number. The jet is able to survive the onset of the more destructive m=1 mode in this way. Our simulations also show that jets can acquire corkscrew or wobbling types of geometries in this relatively stable end state depending on the nature of the perturbations on them. Finally, we suggest that jets go into alternating periods of low and high activity since the disappearance of unstable modes in the sub-Alfv\'{e}nic regime enables another cycle of acceleration to super-Alfv\'{e}nic speeds.},
        author = {Ouyed, R.  and Clarke, D. A.  and Pudritz, R. E. },
        citeulike-article-id = {2802551},
        doi = {10.1086/344507},
        eprint = {astro-ph/0205465},
        journal = {\apj},
        keywords = {2003, clumpyjet-paper},
        month = {January},
        pages = {292--319},
        posted-at = {2008-05-15 20:28:48},
        priority = {2},
        title = {Three-dimensional Simulations of Jets from Keplerian Disks: Self-regulatory Stability},
        url = {http://arxiv.org/abs/astro-ph/0205465},
        volume = {582},
        year = {2003}
}



@article{konigl2004diskwinds,
        abstract = {There have been claims in the literature that accretion disks in which a centrifugally driven wind is the dominant mode of angular momentum transport are inherently unstable. This issue is considered here by applying an equilibrium-curve analysis to the wind-driving, ambipolar diffusion dominated, magnetic-disk model of Wardle and K\"{o}nigl. The equilibrium solution curves for this class of models typically exhibit two distinct branches. It is argued that only one of these branches represents unstable equilibria and that a real disk/wind system likely corresponds to a stable solution.},
        author = {K\"{o}nigl, A. },
        citeulike-article-id = {2802549},
        doi = {10.1086/425648},
        eprint = {astro-ph/0409208},
        journal = {\apj},
        keywords = {2004, clumpyjet-paper},
        month = {December},
        pages = {1267--1271},
        posted-at = {2008-05-15 20:28:13},
        priority = {2},
        title = {Are Magnetic Wind-driving Disks Inherently Unstable?},
        url = {http://arxiv.org/abs/astro-ph/0409208},
        volume = {617},
        year = {2004}
}



@article{golingo2005zpinch,
        abstract = {View this record in Web of Science},
        author = {Golingo, R. P.  and Shumlak, U.  and Nelson, B. A. },
        citeulike-article-id = {2796044},
        journal = {Phys. Plas.},
        keywords = {2005, clumpyjet-paper},
        number = {6},
        posted-at = {2008-05-13 21:01:18},
        priority = {2},
        publisher = {AIP},
        title = {Formation of a sheared flow Z pinch},
        url = {http://scitation.aip.org/getabs/servlet/GetabsServlet?prog=normal\&id=PHPAEN000012000006062505000001\&idtype=cvips\&gifs=yes},
        volume = {12},
        year = {2005}
}



@article{rubini2007obliqueshocks,
        abstract = {Aims.Elongated jets from young stellar objects typically present a nodular structure, formed by a chain of bright knots of enhanced emission with individual proper motions. Though it is generally accepted that internal shocks play an important role in the formation and dynamics of such structures, their precise origin and the mechanisms behind the observed proper motions is still a matter of debate. Our goal is to study numerically the origin, dynamics, and emission properties of such knots. Methods: Axisymmetric simulations are performed with a shock-capturing code for gas dynamics, allowing for molecular, atomic, and ionized hydrogen in non-equilibrium concentrations subject to ionization/recombination processes. Radiative losses in [S ii] lines are computed, and the resulting synthetic emission maps are compared with observations. Results: We show that a pattern of regularly spaced internal oblique shocks, characterized by individual proper motions, is generated by the pressure gradient between the propagating jet and the time variable external cocoon. In the case of under-expanded, light jets the resulting emission knots are found to move downstream with the jet flow, with increasing velocity and decaying brightness toward the leading bow shock. This suggests that the basic properties of the knots observed in stellar jets can be reproduced even without invoking ad hoc pulsating conditions at the jet inlet, though an interplay between the two scenarios is certainly possible.},
        author = {Rubini, F.  and Lorusso, S.  and Del Zanna, L.  and Bacciotti, F. },
        citeulike-article-id = {2796039},
        doi = {10.1051/0004-6361:20077645},
        eprint = {0707.4438},
        journal = {\aap},
        keywords = {2007, clumpyjet-paper},
        month = {September},
        pages = {855--865},
        posted-at = {2008-05-13 20:56:25},
        priority = {2},
        title = {Proper motions of radiative knots in simulations of stellar jets. An alternative to pulsating inflow conditions},
        url = {http://arxiv.org/abs/0707.4438},
        volume = {472},
        year = {2007}
}



@article{masciadri2002sawtooth,
        abstract = {We consider a model for HH 111 as a jet ejected with a sawtooth, time-dependent ejection velocity. Such a variability is suggested by the position-velocity (PV) diagrams obtained from Hubble Space Telescope observations. We calculate both analytic and numerical models describing the flow resulting from such an ejection velocity time variability. Analytically, we calculate the flow for the limiting cases of massless working surfaces (i.e., those that efficiently eject mass sideways into the cocoon of the jet) and mass-conserving working surfaces, and we find that the numerically computed flow lies between these two limits. From the numerical simulations, we compute PV diagrams that can be directly compared with the corresponding observations. We find a surprisingly good agreement, which can be seen as a partial confirmation of the interpretation of the knots along HH 111 as the result of a time dependence in the ejection. Also, we show that a sawtooth functional form for the ejection velocity variability appears to be particularly appropriate for modeling the detailed radial velocity structure of the knots along HH 111. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research, Inc. and under NASA contract NAS5-26555.},
        author = {Masciadri, E.  and Vel\'{a}zquez, P. F.  and Raga, A. C.  and Cant\'{o}, J.  and Noriega-Crespo, A. },
        citeulike-article-id = {2796034},
        doi = {10.1086/340555},
        journal = {\apj},
        keywords = {2002, clumpyjet-paper},
        month = {July},
        pages = {260--269},
        posted-at = {2008-05-13 20:52:15},
        priority = {2},
        title = {Analytic and Numerical Models for the Knots along the HH 111 Jet},
        url = {http://dx.doi.org/10.1086/340555},
        volume = {573},
        year = {2002}
}



@article{masciadri2002precession,
        abstract = {The giant jets represent a fundamental trace of the historical evolution of the outflow activity over timescales of ~10<SUP>4</SUP> yr, i.e., a timescale comparable to the accretion time of the outflow sources in their main protostellar phase. The study of such huge jets provides the possibility of retrieving important elements related to the life of the outflow sources. In this paper, we study the role of precession (combined with jet velocity variability and the resulting enhanced interaction with the surrounding environment) as a deceleration mechanism for giant jets, using a numerical approach. This thesis was proposed for the first time by Devine et al., but it could not be numerically explored until now, because it is intrinsically difficult to reproduce, at the same time, the large range of scales from ~100 AU up to a few parsecs. In the present paper, we obtain predictions of Halpha intensity maps and position-velocity diagrams from three-dimensional simulations of the giant HH 34 jet (including an appropriate ejection velocity time variability and a precession of the outflow axis), and we compare them with previously published observations of this object. Our simulations represent a step forward from previous numerical studies of HH objects, in that the use of a seven-level, binary adaptive grid has allowed us to compute models that appropriately cover all relevant scales of a giant jet, from the ~100 AU jet radius close to the source to the ~1 pc length of the outflow. A good qualitative and quantitative agreement is found between the model predictions and the observations, indicating that a precession of the jet axis can indeed be the probable cause of the deceleration of the giant jets. Moreover, we show that a critical parameter for obtaining a better or worse agreement with the observations is the ratio rho<SUB>j</SUB>/rho<SUB>a</SUB> between the jet and the environmental densities. The implications of this result in the context of the current star formation models are discussed.},
        author = {Masciadri, E.  and de Gouveia Dal Pino, E. M. and Raga, A. C.  and Noriega-Crespo, A. },
        citeulike-article-id = {2796031},
        doi = {10.1086/343797},
        eprint = {astro-ph/0208277},
        journal = {\apj},
        keywords = {2002, clumpyjet-paper},
        month = {December},
        pages = {950--958},
        posted-at = {2008-05-13 20:49:36},
        priority = {2},
        title = {The Precession of the Giant HH 34 Outflow: A Possible Jet Deceleration Mechanism},
        url = {http://arxiv.org/abs/astro-ph/0208277},
        volume = {580},
        year = {2002}
}



@article{lebedev2005labjet,
        author = {Lebedev, S. V.  and Ciardi, A.  and Ampleford, D. J.  and Bland, S. N.  and Bott, S. C.  and Chittenden, J. P.  and Hall, G. N.  and Rapley, J.  and Jennings, C. A.  and Frank, A.  and Blackman, E. G.  and Lery, T. },
        citeulike-article-id = {247383},
        doi = {10.1111/j.1365-2966.2005.09132.x},
        eprint = {astro-ph/0505027},
        issn = {0035-8711},
        journal = {\mnras},
        keywords = {2005, clumpyjet-paper, lab},
        month = {July},
        number = {1},
        pages = {97--108},
        posted-at = {2008-05-13 20:45:47},
        priority = {2},
        publisher = {Blackwell Publishing},
        title = {Magnetic tower outflows from a radial wire array Z-pinch},
        url = {http://arxiv.org/abs/astro-ph/0505027},
        volume = {361},
        year = {2005}
}



@article{miniati2007amr,
        abstract = {We present a new numerical algorithm for the solution of coupled collisional and collisionless systems, based on the block structured adaptive mesh and time refinement strategy (AMR). We describe the issues associated with the discretization of the system equations and the synchronization of the numerical solution on the hierarchy of grid levels. We implement a code based on a higher order, conservative and directionally unsplit Godunov's method for hydrodynamics; a symmetric, time centered modified symplectic scheme for collisionless component; and a multilevel, multigrid relaxation algorithm for the elliptic equation coupling the two components. Numerical results that illustrate the accuracy of the code and the relative merit of various implemented schemes are also presented.},
        author = {Miniati, Francesco   and Colella, Phillip  },
        citeulike-article-id = {2796019},
        doi = {10.1016/j.jcp.2007.07.035},
        journal = {J. Comp. Phys.},
        keywords = {2007, amr, elliptic},
        month = {November},
        number = {1},
        pages = {400--430},
        posted-at = {2008-05-13 20:40:56},
        priority = {2},
        title = {Block structured adaptive mesh and time refinement for hybrid, hyperbolic + N-body systems},
        url = {http://dx.doi.org/10.1016/j.jcp.2007.07.035},
        volume = {227},
        year = {2007}
}



@article{klein1994,
        abstract = {The interstellar medium (ISM) is inhomogeneous, with clouds of various temperatures and densities embedded in a tenuous intercloud medium. Shocks propagating through the ISM can ablate or destroy the clouds, at the same time significantly altering the properties of the intercloud medium. This paper presents a comprehensive numerical study of the simplest case of the interaction between a shock wave and a spherical cloud, in which the shock far from the cloud is steady and planar, and in which radiative losses, thermal conduction, magnetic fields, and gravitational forces are all neglected. As a result, the problem is completely specified by two numbers: the Mach number of the shock, M, and the ratio of the density of the cloud to that of the intercloud medium, Chi. For strong shocks we show that the dependence on M scales out, so the primary independent parameter is Chi. Variations from this simple case are also considered: the potential effect of radiative losses is assessed by calculations in which the ratio of specific heats in the cloud is 1.1 instead of 5/3; the effect of the initial shape of the cloud is studied by using a cylindrical cloud instead of a spherical one; and the role of the initial shock is determined by considering the case of a cloud embedded in a wind. Local adaptive mesh refinement techniques with a second-order, two-fluid, two-dimensional Godunov hydrodynamic scheme are used to address these problems, allowing heretofore unobtainable numerical resolution. Convergence studies to be described in a subsequent paper demonstrate that about 100 zones per cloud radius are needed for accurate results; previous calculations have generally used about a third of this number. The results of the calculations are analyzed in terms of global quantities which provide an overall description of te shocked cloud: the size and shape of the cloud, the mean density, the mean pressure, the mean velocity, the velocity dispersion, and the total circulation.},
        author = {Klein, R. I.  and Mckee, C. F.  and Colella, P. },
        citeulike-article-id = {2795994},
        doi = {10.1086/173554},
        journal = {\apj},
        keywords = {1994, clumps, clumpyjet-paper},
        month = {January},
        pages = {213--236},
        posted-at = {2008-05-13 20:13:48},
        priority = {2},
        title = {On the hydrodynamic interaction of shock waves with interstellar clouds. 1: Nonradiative shocks in small clouds},
        url = {http://dx.doi.org/10.1086/173554},
        volume = {420},
        year = {1994}
}



@article{fragile2005mhdclumps,
        abstract = {We present results from two-dimensional numerical simulations of the interactions between magnetized shocks and radiative clouds. Our primary goal is to characterize the dynamical evolution of the shocked clouds. We perform runs in both the strong and weak magnetic field limits and consider three different field orientations. For the geometries considered, we generally find that magnetic fields external to, but concentrated near, the surface of the cloud suppress the growth of destructive hydrodynamic instabilities. External fields also increase the compression of the cloud by effectively acting as a confinement mechanism driven by the interstellar flow and local field stretching. This can have a dramatic effect on both the efficiency of radiative cooling, which tends to increase with increasing magnetic field strength, and on the size and distribution of condensed cooled fragments. In contrast, fields acting predominately internally to the cloud tend to resist compression, thereby inhibiting cooling. We observe that, even at modest strengths (beta<SUB>0</SUB><~100), internal fields can completely suppress low-temperature (T<100 K) cooling in two-dimensional clouds.},
        author = {Fragile, P. C.  and Anninos, P.  and Gustafson, K.  and Murray, S. D. },
        citeulike-article-id = {2795978},
        doi = {10.1086/426313},
        eprint = {astro-ph/0410285},
        journal = {\apj},
        keywords = {2005, clumps, clumpyjet-paper, mhd},
        month = {January},
        pages = {327--339},
        posted-at = {2008-05-13 20:04:02},
        priority = {2},
        title = {Magnetohydrodynamic Simulations of Shock Interactions with Radiative Clouds},
        url = {http://arxiv.org/abs/astro-ph/0410285},
        volume = {619},
        year = {2005}
}



@article{fragile2004,
        abstract = {Accumulating observational evidence for a number of radio galaxies suggests an association between their jets and regions of active star formation. The standard picture is that shocks generated by the jet propagate through an inhomogeneous medium and trigger the collapse of overdense clouds, which then become active star-forming regions. In this contribution, we report on recent hydrodynamic simulations of radiative shock-cloud interactions using two different cooling models: an equilibrium cooling-curve model assuming solar metallicities and a non-equilibrium chemistry model appropriate for primordial gas clouds. We consider a range of initial cloud densities and shock speeds in order to quantify the role of cooling in the evolution. Our results indicate that for moderate cloud densities (>1 cm^-3) and shock Mach numbers (<20), cooling processes can be highly efficient and result in more than 50\% of the initial cloud mass cooling to below 100 K. We also use our results to estimate the final H\_2 mass fraction for the simulations that use the non-equilibrium chemistry package. This is an important measurement, since H\_2 is the dominant coolant for a primordial gas cloud. We find peak H\_2 mass fractions of >0.01 and total H\_2 mass fractions of >10^-5 for the cloud gas. Finally, we compare our results with the observations of jet-induced star formation in “Minkowski's Object.” We conclude that its morphology, star formation rate (~ 0.3M\_solar/yr) and stellar mass (~ 1.2 x 10^7 M\_solar) can be explained by the interaction of a 90,000 km/s jet with an ensemble of moderately dense (~ 10 cm^-3), warm (10^4 K) intergalactic clouds in the vicinity of its associated radio galaxy at the center of the galaxy cluster.},
        author = {Fragile, Chris  P.  and Murray, Stephen  D.  and Anninos, Peter   and van Breugel, Wil  },
        citeulike-article-id = {692675},
        doi = {10.1086/381726},
        eprint = {astro-ph/0311298},
        journal = {\apj},
        keywords = {2004, clumps, clumpyjet-paper},
        month = {March},
        pages = {74--87},
        posted-at = {2008-05-13 19:57:45},
        priority = {2},
        title = {Radiative Shock-Induced Collapse of Intergalactic Clouds},
        url = {http://arxiv.org/abs/astro-ph/0311298},
        volume = {604},
        year = {2004}
}



@article{ciardi2008curved,
        abstract = {Herbig-Haro jets often show some degree of curvature along their path, in many cases produced by the ram pressure of a side wind. We present simulations of both laboratory and astrophysical curved jets and results from laboratory experiments. We discuss the properties and similarities of the laboratory and astrophysical flows, which show the formation of internal shocks and working surfaces. In particular, the results illustrate how the breakup of the bow shock and clumps in the flow are produced without invoking jet variability; we also discuss how jet rotation reduces the growth of the Rayleigh-Taylor instability in curved jets.},
        author = {Ciardi, A.  and Ampleford, D. J.  and Lebedev, S. V.  and Stehle, C. },
        citeulike-article-id = {2795965},
        doi = {10.1086/528679},
        eprint = {0712.0959},
        journal = {Astrophys. J.},
        keywords = {2008, clumpyjet-paper, lab},
        month = {May},
        pages = {968--973},
        posted-at = {2008-05-13 19:54:13},
        priority = {2},
        title = {Curved Herbig-Haro Jets: Simulations and Experiments},
        url = {http://arxiv.org/abs/0712.0959},
        volume = {678},
        year = {2008}
}

@ARTICLE{collins2005,
   author = {{Collins}, T.~J.~B. and {Poludnenko}, A. and {Cunningham}, A. and 
        {Frank}, A.},
    title = "{Shock propagation in deuterium-tritium-saturated foam}",
  journal = {Physics of Plasmas},
 keywords = {Shock waves and discontinuities, Magnetohydrodynamic and fluid equation, Fluctuation and chaos phenomena, Transport properties, Plasma turbulence},
     year = 2005,
    month = jun,
   volume = 12,
   number = 6,
    pages = {062705-+},
      doi = {10.1063/1.1927099},
   adsurl = {http://adsabs.harvard.edu/abs/2005PhPl...12f2705C},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}



@article{ciardi2007labjet,
        abstract = {The evolution of laboratory produced magnetic jets is followed numerically through three-dimensional, nonideal magnetohydrodynamic simulations. The experiments are designed to study the interaction of a purely toroidal field with an extended plasma background medium. The system is observed to evolve into a structure consisting of an approximately cylindrical magnetic cavity with an embedded magnetically confined jet on its axis. The supersonic expansion produces a shell of swept-up shocked plasma that surrounds and partially confines the magnetic tower. Currents initially flow along the walls of the cavity and in the jet but the development of current-driven instabilities leads to the disruption of the jet and a rearrangement of the field and currents. The top of the cavity breaks up, and a well-collimated, radiatively cooled, “clumpy” jet emerges from the system.},
        author = {Ciardi, A.  and Lebedev, S. V.  and Frank, A.  and Blackman, E. G.  and Chittenden, J. P.  and Jennings, C. J.  and Ampleford, D. J.  and Bland, S. N.  and Bott, S. C.  and Rapley, J.  and Hall, G. N.  and Suzuki-Vidal, F. A.  and Marocchino, A.  and Lery, T.  and Stehle, C. },
        citeulike-article-id = {2795963},
        doi = {10.1063/1.2436479},
        eprint = {astro-ph/0611441},
        journal = {Phys. Plas.},
        keywords = {2007, clumpyjet-paper, lab},
        month = {May},
        pages = {6501},
        posted-at = {2008-05-13 19:53:51},
        priority = {2},
        title = {The evolution of magnetic tower jets in the laboratory},
        url = {http://arxiv.org/abs/astro-ph/0611441},
        volume = {14},
        year = {2007}
}



@article{raga2002hh34/111,
        abstract = {The southern lobe of HH 34 and the western lobe of HH 111 show remarkable similarities. Both objects have a chain of well aligned knots, ending in well defined bow shocks (HH 34S and HH 111V, respectively). In this paper, we derive the past ejection velocity histories from previously published radial velocity measurements of the HH 34 and HH 111 jets. This is done under the assumption that the flows are ballistic. From these reconstructed ejection velocity variabilities, we compute axisymmetric gasdynamic simulations of the two flows, and find that we do obtain large working surfaces at the positions of the HH 34S and HH 111V bow shocks for the time at which these objects are being observed. This appears to be quite definite proof that these bow shocks are indeed the result of an ejection velocity time-variability. Also, there is the observational fact that the HH 34S bow shock is huge, being wider than HH 111V by a factor of ~ 3. We find that we can reproduce this difference in size by choosing an appropriate value for the density of the ambient medium. Finally, from our small sample of two reconstructed ejection velocity variability histories, we attempt to make some statements about the general nature of these variabilites, and their implications on the possible ejection/collimation mechanisms.},
        author = {Raga, A. C.  and Vel\'{a}zquez, P. F.  and Cant\'{o}, J.  and Masciadri, E. },
        citeulike-article-id = {2783478},
        doi = {10.1051/0004-6361:20021180},
        journal = {\aap},
        keywords = {2002, hh-111, hh-34, jetclump-paper},
        month = {November},
        pages = {647--656},
        posted-at = {2008-05-11 00:25:44},
        priority = {0},
        title = {The time-dependent ejection velocity histories of HH 34 and HH 111},
        url = {http://dx.doi.org/10.1051/0004-6361:20021180},
        volume = {395},
        year = {2002}
}



@article{decolle2005,
        author = {De Colle, F.  and Raga, A. C. },
        citeulike-article-id = {166035},
        doi = {10.1111/j.1365-2966.2005.08876.x},
        issn = {0035-8711},
        journal = {\mnras},
        keywords = {2005, jetclump-paper},
        month = {May},
        number = {1},
        pages = {164--170},
        posted-at = {2008-05-09 21:32:54},
        priority = {1},
        publisher = {Blackwell Publishing},
        title = {Interaction of Herbig-Haro objects with molecular cloud and generation of Alfven waves},
        url = {http://dx.doi.org/10.1111/j.1365-2966.2005.08876.x},
        volume = {359},
        year = {2005}
}



@article{dalpino1999,
        abstract = {We report the results of three-dimensional smoothed particle hydrodynamics simulations of interactions of overdense, radiatively cooling and adiabatic jets with dense, compact clouds in frontal and off-axis collisions. Calculated for a set of parameters that are particularly appropriate to protostellar jets, our results indicate that the interaction produces important transient and permanent effects in the jet morphology. In off-axis interactions, the deflected beam initially describes a C-shaped trajectory around the curved jet/cloud contact discontinuity, but the deflection angle tends to decrease with time as the beam slowly penetrates the cloud. Later, when the jet has penetrated most of the cloud extension, the deflected beam fades and the jet resumes its original direction of propagation. During the interaction, a weak chain of internal knots develops along the deflected beam and the velocity field initially has a complex structure that later evolves to a more uniform distribution. The average velocity of the deflected beam is consistent with the predicted value given by v<SUP>'</SUP><SUB>j</SUB>~=v<SUB>j</SUB>costheta (where theta is the deflection angle and v<SUB>j</SUB> is the velocity of the incident beam). The impact also decreases the beam collimation. Applied to the context of the protostellar jets, this morphology and kinematics found for the deflected beam is very similar to that observed in some candidate systems like the HH 110 jet, which has been previously proposed to be the deflected part of the HH 270 jet. Our simulations also reveal the formation of a head-neck bright structure at the region of impact that resembles the morphology of the HH 110 knot A located in the apex of the HH 110 jet, where the deflection is believed to occur. All these similarities strongly support the proposed jet/cloud interaction interpretation for this system. The fact that the deflection angles derived from the simulations are smaller than that observed and the fact that the jet/cloud interaction is still taking place indicate that the interacting cloud in that system must have a radius R<SUB>c</SUB>>>R<SUB>j</SUB>, where R<SUB>j</SUB>\& is the jet radius, as previously suggested, and a density ratio between the jet and the cloud beta<SUP>2</SUP>=n<SUB>j</SUB>/n<SUB>c</SUB><~10<SUP>-2</SUP>. Because of the small size of the clouds [with radius R<SUB>c</SUB>~=(1-2)R<SUB>j</SUB>], the interactions examined here are very transient (with lifetimes of few ~10 to ~100 yr that are much less than the typical dynamical lifetimes of the protostellar outflows, tau>~10<SUP>4</SUP> yr). Nonetheless, they leave important signatures in the surviving outflow. The leftovers of the cloud and the knots that are produced in the deflected beam are deposited into the working surface and contribute to enrich the knotty pattern commonly observed in Herbig-Haro objects behind the bow shocks of protostellar jets. Also, the collision may partially destroy the shell at the head, producing remarkable asymmetries in the head region. A jet undergoing many transient interactions with compact clumps along its propagation and lifetime may inject a considerable amount of shocked jet material sideways into the surrounding ambient medium, and this process may provide a powerful tool for momentum transfer and turbulent mixing with the ambient medium.},
        author = {de Gouveia Dal Pino, E. M.},
        citeulike-article-id = {2776580},
        doi = {10.1086/308037},
        eprint = {astro-ph/9904145},
        journal = {\apj},
        keywords = {1999, 3d, clumpyjet-paper, de-gouveia-dal-pino, jetclump-paper, jets, sph},
        month = {December},
        pages = {862--873},
        posted-at = {2008-05-09 21:31:20},
        priority = {0},
        title = {Three-dimensional Simulations of Jet/Cloud Interactions: Structure and Kinematics of the Deflected Jets},
        url = {http://arxiv.org/abs/astro-ph/9904145},
        volume = {526},
        year = {1999}
}



@article{cabrit2000hh34,
        abstract = {The HH 34 superjet shows a steep velocity decrease (from ~500 to ~100 km s^-1) over a distance of ~2 pc on either side of the central source. We explore whether or not this behaviour could be interpreted as evidence for a slow "turning on" of the ejection velocity of the jet, and find that this is indeed possible, but only for an ejection velocity that has had a dramatic growth over the last 10^4 yr, and is just about to stabilize within the next 4000 yr. We argue that such a time-variability is somewhat unlikely. We then explore a second scenario, in which the slowing down of the HH 34 superjet is modeled as the result of the interaction of a fragmented jet with the surrounding environment. We find that for parameters appropriate for HH 34, this model does appear to reproduce the observed slowing down of the superjet in a natural way. We therefore conclude that the kinematical properties of the HH 34 superjet are most likely to be the result of environmental drag on the propagation of individual jet knots, resulting from the fragmentation of a time-variable, precessing jet.},
        author = {Cabrit, Sylvie   and Raga, Alex  },
        citeulike-article-id = {2776577},
        journal = {\aap},
        keywords = {2000, cabrit, clumpyjet-paper, hh-34},
        pages = {667--673},
        posted-at = {2008-05-09 21:28:46},
        priority = {1},
        title = {Theoretical interpretation of the apparent deceleration in the HH 34 superjet},
        url = {http://aa.springer.de/bibs/0354002/2300667/small.htm},
        volume = {354},
        year = {2000}
}



@article{blondin1990,
        abstract = {The two-dimensional simulations presently used to characterize the structure and evolution of radiatively cooling supersonic jets reveal that cooling jet morphologies resemble those of adiabatic outflows, but with the fundamental difference that a dense, cold shell will condense out of the shocked gas at the head of the jet when the cooling distance behind either of the two principal shocks is smaller than the jet radius. For very high cooling rates, the material that accumulates at the head of the jet forms an extended plug of cold gas resembling the 'nose cone' observed in numerical simulations of strongly magnetized adiabatic jets. An investigation is made of the dependence of jet properties on the density ratio between the beam and the ambient medium, as well as on the strength of radiative cooling.},
        author = {Blondin, J. M.  and Fryxell, B. A.  and Konigl, A. },
        citeulike-article-id = {2776566},
        doi = {10.1086/169128},
        journal = {\apj},
        keywords = {1990, clumpyjet-paper, jetclump-paper, jets},
        month = {September},
        pages = {370--386},
        posted-at = {2008-05-09 21:23:19},
        priority = {0},
        title = {The structure and evolution of radiatively cooling jets},
        url = {http://dx.doi.org/10.1086/169128},
        volume = {360},
        year = {1990}
}



@article{bally2002hh1/2,
        abstract = {Hubble Space Telescope observations obtained in 1994 and 1997 are used to measure proper motions in the HH 1/2 protostellar outflow in Orion. Since the HH 1/2 system lies within 10° of the plane of the sky, proper motions provide accurate measures of true space velocities. Comparison of the 1994 and 1997 images reveals a variety of changes such as the emergence of new knots from the driving source embedded in the HH 1/2 cloud core and the fading or brightening of some features. However, such brightness changes affect a small fraction (<10\%) of the total emission. Proper motion measurements reveal complex velocity variations along the flow axis and pronounced velocity shear orthogonal to it. Along the extension of the HH 1 jet axis, speeds vary from under 100 km s<SUP>-1</SUP> near the tip of HH 2, range from 255 to 345 km s<SUP>-1</SUP> in the HH 1 jet itself, and reach peak values of more than 400 km s<SUP>-1</SUP> near the leading edge of HH 1 and in parts of the brightest knot complexes in the center of HH 2. While the velocity dispersion within the low-excitation HH 1 jet is less than 30 km s<SUP>-1</SUP>, high-excitation features in HH 1 and HH 2 exhibit local velocity variations in excess of 150 km s<SUP>-1</SUP>. Both the internal velocity dispersion and the angular width of the emitting fluid as seen from the source, VLA 1, increase with distance. HH 1 and HH 2 contain complex substructures having chaotic internal motions, proper motions that decline rapidly orthogonal to the jet axis, and both downstream- and upstream-facing (reverse) bow shocks. Downstream-facing bow features tend to have high velocities, while reverse-facing bow shocks have low speeds. The complex texture and flow field indicate that both the fast and slow fluid elements now colliding in shocks were clumped and had chaotic velocity fields prior to entering the currently active shocks. Both fluids may have been processed by prior generations of shocks and by instabilities. Indeed, transverse motions in HH 1 and HH 2 indicate that expansion started well after the material was ejected from VLA 1, possibly as a result of having been processed through now extinct shocks. A second outflow from the HH 1/2 cloud core, HH 501, which consists of two knots located about 1" west of the base of the HH 1 jet, also has proper motions directly away from VLA 1, but with a speed of only about 180 km s<SUP>-1</SUP>. The lack of interactions between the nearby high-speed HH 1 and slower HH 501 jets may indicate that the density of the medium surrounding each jet is at least an order of magnitude below that of the visible knots. Thus, the visible jet components probably transport the bulk of the energy and momentum in these outflows. Finally, the Cohen-Schwartz star is found to be a 0.2" separation binary.},
        author = {Bally, J.  and Heathcote, S.  and Reipurth, B.  and Morse, J.  and Hartigan, P.  and Schwartz, R. },
        citeulike-article-id = {2776564},
        doi = {10.1086/339837},
        journal = {\aj},
        keywords = {2002, bally, clumpyjet-paper, hh-1, hh-2, jetclump-paper},
        month = {May},
        pages = {2627--2657},
        posted-at = {2008-05-09 21:22:34},
        priority = {0},
        title = {Hubble Space Telescope Observations of Proper Motions in Herbig-Haro Objects 1 and 2},
        url = {http://dx.doi.org/10.1086/339837},
        volume = {123},
        year = {2002}
}



@article{poludnenko2002,
        abstract = {Many astrophysical flows occur in inhomogeneous (clumpy) media. We present results of a numerical study of steady, planar shocks interacting with a system of embedded cylindrical clouds. Our study uses a two-dimensional geometry. Our numerical code uses an adaptive mesh refinement, allowing us to achieve sufficiently high resolution both at the largest and the smallest scales. We neglect any radiative losses, heat conduction, and gravitational forces. Detailed analysis of the simulations shows that interaction of embedded inhomogeneities with the shock/postshock wind depends primarily on the thickness of the cloud layer and arrangement of the clouds in the layer. The total cloud mass and the total number of individual clouds is not a significant factor. We define two classes of cloud distributions: thin and thick layers. We define the critical cloud separation along the direction of the flow and perpendicular to it, distinguishing between the interacting and noninteracting regimes of cloud evolution. Finally, we discuss mass loading and mixing in such systems.},
        author = {Poludnenko, A. Y.  and Frank, A.  and Blackman, E. G. },
        citeulike-article-id = {2776549},
        doi = {10.1086/341886},
        eprint = {astro-ph/0109282},
        journal = {\apj},
        keywords = {2002, clumps, clumpyjet-paper, poludnenko},
        month = {September},
        pages = {832--848},
        posted-at = {2008-05-09 21:16:05},
        priority = {0},
        title = {Hydrodynamic Interaction of Strong Shocks with Inhomogeneous Media. I. Adiabatic Case},
        url = {http://arxiv.org/abs/astro-ph/0109282},
        volume = {576},
        year = {2002}
}



@article{poludnenko2004,
        abstract = {We present a design for high energy density laboratory experiments studying the interaction of hypersonic shocks with a large number of inhomogeneities. These “clumpy” flows are relevant to a wide variety of astrophysical environments, including the evolution of molecular clouds, outflows from young stars, planetary nebulae, and active galactic nuclei. The experiment consists of a strong shock (driven by a pulsed-power machine or a high-intensity laser) impinging on a region of randomly placed plastic rods. We discuss the goals of the specific design and how they are met by specific choices of target components. An adaptive mesh refinement hydrodynamic code is used to analyze the design and establish a predictive baseline for the experiments. The simulations confirm the effectiveness of the design in terms of articulating the differences between shocks propagating through smooth and clumpy environments. In particular, we find significant differences between the shock propagation speeds in a clumpy medium and those in a smooth one with the same average density. The simulation results are of general interest for foams in both inertial confinement fusion and laboratory astrophysics studies. Our results highlight the danger of using average properties of inhomogeneous astrophysical environments when comparing timescales for critical processes, such as shock crossing and gravitational collapse.},
        author = {Poludnenko, A. Y.  and Dannenberg, K. K.  and Drake, R. P.  and Frank, A.  and Knauer, J.  and Meyerhofer, D. D.  and Furnish, M.  and Asay, J. R.  and Mitran, S. },
        citeulike-article-id = {2776546},
        doi = {10.1086/381792},
        eprint = {astro-ph/0305146},
        journal = {\apj},
        keywords = {2004, lab, poludnenko},
        month = {March},
        pages = {213--221},
        posted-at = {2008-05-09 21:15:26},
        priority = {0},
        title = {A Laboratory Investigation of Supersonic Clumpy Flows: Experimental Design and Theoretical Analysis},
        url = {http://arxiv.org/abs/astro-ph/0305146},
        volume = {604},
        year = {2004}
}



@article{cunningham2005waw,
        abstract = {We carry out high-resolution simulations of the inner regions of a wide-angle wind-driven bipolar outflow using an adaptive mesh refinement code. Our code follows H-He gas with molecular, atomic, and ionic components and the associated time-dependent molecular chemistry and ionization dynamics with radiative cooling. Our simulations explore the nature of the outflow when a spherical wind expands into a rotating, collapsing envelope. We compare these with key observational properties of the outflow system of source I in the BN/KL region. Our calculations show that the wind evacuates a bipolar outflow cavity in the infalling envelope. We find the head of the outflow to be unstable and that it rapidly fragments into clumps. We resolve the dynamics of the strong shear layer, which defines the side walls of the cavity. We conjecture that this layer is the likely site of maser emission and examine its morphology and rotational properties. The shell of swept-up ambient gas that delineates the cavity edge retains its angular momentum. This rotation is roughly consistent with that observed in the source I SiO maser spots. The observed proper motions and line-of-sight velocity are approximately reproduced by the model. The cavity shell at the base of the flow assumes an X-shaped morphology that is also consistent with source I. We conclude that the wide opening angle of the outflow is evidence that a wide-angle wind drives the source I outflow and not a collimated jet.},
        author = {Cunningham, A.  and Frank, A.  and Hartmann, L. },
        citeulike-article-id = {2776539},
        doi = {10.1086/432658},
        eprint = {astro-ph/0506159},
        journal = {\apj},
        keywords = {2005, andy, astrobear, cooling},
        month = {October},
        pages = {1010--1021},
        posted-at = {2008-05-09 21:11:20},
        priority = {2},
        title = {Wide-Angle Wind-driven Bipolar Outflows: High-Resolution Models with Application to Source I of the Becklin-Neugebauer/Kleinmann-Low OMC-I Region},
        url = {http://arxiv.org/abs/astro-ph/0506159},
        volume = {631},
        year = {2005}
}



@article{cunningham2006collisions,
        abstract = {We present a series of numerical studies of the interaction of colliding radiative, hydrodynamic young stellar outflows. We study the effect of the collision impact parameter on the acceleration of ambient material and the degree to which the flow is isotropized by the collision as a mechanism for driving turbulence in the parent molecular cloud. Our results indicate that the high degree of compression of outflow material, achieved through radiative shocks near the vertex of the interaction, prevents the redirected outflow from spraying over a large spatial region. Furthermore, the collision reduces the redirected outflow's ability to entrain and impart momentum into the ambient cloud. Consideration of the probabilities of outflow collisions leads us to conclude that individual low-velocity fossil outflows are the principle coupling between outflows and the cloud.},
        author = {Cunningham, A. J.  and Frank, A.  and Blackman, E. G. },
        citeulike-article-id = {2776535},
        doi = {10.1086/505132},
        eprint = {astro-ph/0512490},
        journal = {\apj},
        keywords = {2006, andy, jets},
        month = {August},
        pages = {1059--1069},
        posted-at = {2008-05-09 21:10:43},
        priority = {2},
        title = {Protostellar Jet Collisions Reduce the Efficiency of Outflow-Driven Turbulence in Molecular Clouds},
        url = {http://arxiv.org/abs/astro-ph/0512490},
        volume = {646},
        year = {2006}
}



@article{cunningham2006cavities,
        abstract = {We investigate the evolution of fossil cavities produced by extinct young stellar object (YSO) jets and wide-angle outflows. Fossil cavities are ellipsoidal or cylindrical shells of swept-up ambient (molecular cloud) material moving at low velocities. The cavities form when the momentum in a YSO jet or wide-angle outflow decays in time, allowing the bow shock or swept-up shell to decelerate to velocities near the turbulent speed in the cloud. It has been suggested in previous studies that cavities provide efficient coupling between the jets/outflows and the cloud and, as such, are the agents by which cloud turbulence can be re-energized. In this paper, we carry forward a series of numerical simulations of jets and outflows whose momentum flux decreases in time. We compare simulations with decaying momentum fluxes to those with constant flux. We show that decaying flux models exhibit deceleration of the outflow head and back-filling via expansion off of the cavity walls. They also have lower density contrast and are longer lived and wider than their continuously driven counterparts. The simulations recover the basic properties of observed fossil cavities. In addition, we provide synthetic observations in terms of position-velocity (PV) diagrams, which demonstrate that fossil cavities form both jets and wide-angle outflows and are characterized by linear “Hubble law” expansion patterns superimposed on “spur” patterns, indicative of the head of a bow shock.},
        author = {Cunningham, A. J.  and Frank, A.  and Quillen, A. C.  and Blackman, E. G. },
        citeulike-article-id = {2776533},
        doi = {10.1086/508762},
        eprint = {astro-ph/0603014},
        journal = {\apj},
        keywords = {andy, pv-diagrams},
        month = {December},
        pages = {416--424},
        posted-at = {2008-05-09 21:05:42},
        priority = {2},
        title = {Outflow-driven Cavities: Numerical Simulations of Intermediaries of Protostellar Turbulence},
        url = {http://arxiv.org/abs/astro-ph/0603014},
        volume = {653},
        year = {2006}
}



@article{cunningham2007amrmhd,
        abstract = {A description is given of the algorithms implemented in the AstroBEAR adaptive mesh refinement code for ideal magnetohydrodynamics. The code provides several high resolution, shock capturing schemes which are constructed to maintain conserved quantities of the flow in a finite volume sense. Divergence free magnetic field topologies are maintained to machine precision by collating the components of the magnetic field on a cell-interface staggered grid and utilizing the constrained transport approach for integrating the induction equations. The maintenance of such topologies on adaptive grids is achieved using prolongation and restriction operators which preserve the divergence and curl of the magnetic field across co-located grids of different resolution. The robustness and correctness of the code is demonstrated by comparing the numerical solution of various tests with analytical solutions or previously published numerical solutions obtained by other codes.},
        author = {Cunningham, A. J.  and Frank, A.  and Varniere, P.  and Mitran, S.  and Jones, T. W. },
        citeulike-article-id = {2776532},
        eprint = {0710.0424},
        journal = {ArXiv:astro-ph/0710.0424},
        keywords = {amr, andy, astrobear, mhd},
        month = {October},
        posted-at = {2008-05-09 21:04:30},
        priority = {2},
        title = {Simulating Magnetohydrodynamical Flow with Constrained Transport and Adaptive Mesh Refinement; Algorithms \amp Tests of the AstroBEAR Code},
        url = {http://arxiv.org/abs/0710.0424},
        volume = {710},
        year = {2007}
}



@article{homer2004,
        abstract = {We report the results of a 45 ks Chandra observation of the cataclysmic variable (CV) V426 Ophiuchus. The high-resolution spectrum from the high-energy transmission grating spectrometer is most consistent with a cooling flow model, placing V426 Oph among the group of CVs including U Gem and EX Hya. An uninterrupted light curve was also constructed, in which we detect a significant 4.2 hr modulation together with its first harmonic at 2.1 hr. Reanalysis of archival Ginga and ROSAT X-ray light curves also reveals modulations at periods consistent with 4.2 and/or 2.1 hr. Furthermore, optical photometry in V, simultaneous with the Chandra observation, indicates a modulation anticorrelated with the X-ray, and later more extensive R-band photometry finds a signal at ~2.1 hr. The earlier reported X-ray periods at ~0.5 and 1 hr appear to be only transient and quasi-periodic in nature. In contrast, the 4.2 hr period or its harmonic is stable and persistent in X-ray/optical data from 1988 to 2003. This periodicity is clearly distinct from the 6.85 hr orbit and could be due to the spin of the white dwarf. If this is the case, V426 Oph would be the first long-period intermediate polar with a ratio P<SUB>spin</SUB>/P<SUB>orb</SUB> of 0.6. However, this interpretation requires unreasonable values of magnetic field strength and mass accretion rate.},
        author = {Homer, L.  and Szkody, P.  and Raymond, J. C.  and Fried, R. E.  and Hoard, D. W.  and Hawley, S. L.  and Wolfe, M.  and Tramposch, J. N.  and Yirak, K. T. },
        citeulike-article-id = {2776529},
        doi = {10.1086/421864},
        eprint = {astro-ph/0404289},
        journal = {\apj},
        keywords = {mine},
        month = {August},
        pages = {991--1000},
        posted-at = {2008-05-09 21:02:39},
        priority = {1},
        title = {Chandra Observation of V426 Ophiuchi: Weighing the Evidence for a Magnetic White Dwarf},
        url = {http://arxiv.org/abs/astro-ph/0404289},
        volume = {610},
        year = {2004}
}