Gravo-Turbulence

References

• ​Abel et al 2002
• ​Ballesteros-Paredes 1999 Clouds as Turbulent Density Fluctuations: Implications for Pressure Confinement and Spectral Line Data Interpretation
• ​Ballesteros-Paredes 1999 Turbulent Flow-driven Molecular Cloud Formation: A Solution to the Post-T Tauri Problem?
• ​Ballesteros-Paredes 2003 Dynamic cores in hydrostatic disguise
  • SPH Turbulent driving of various sorts with self-gravity turned on. (Periodic BC) 205,379 particles
• ​Ballesteros-Paredes 2006 The Mass Spectra of Cores in Turbulent Molecular Clouds and Implications for the Initial Mass Function
• ​Ballesteros-Paredes 2006 Six myths on the virial theorem for interstellar clouds
• ​Ballesteros-Paredes 2007
• ​Ballesteros-Paredes 2011 Gravity or turbulence? Velocity dispersion-size relation
• ​Ballesteros-Paredes 2011 Gravity or turbulence? II. Evolving column density PDFs in molecular clouds
• ​Banerjee et al 2009 Clump morphology and evolution in MHD simulations of molecular cloud formation
• ​Bate 1998 Collapse of a Molecular Cloud Core to Stellar Densities: The First Three-dimensional Calculations
• ​Bonazzola et al, 1987 Jeans collapse in a turbulent medium
• ​Bonnell and Bate 2006 Star formation through gravitational collapse and competitive accretion
• ​Bonnell and Bate 2006 The Jeans mass and the origin of the knee in the IMF
• ​Boss 1980 Protostellar formation in rotating interstellar clouds. I - Numerical methods and tests
• ​Boss 1980 Protostellar formation in rotating interstellar clouds. II - Axially symmetric collapse
• ​Boss 1980 Protostellar formation in rotating interstellar clouds. III - Nonaxisymmetric collapse
• ​Boss 1984 Protostellar formation in rotating interstellar clouds. IV Nonisothermal collapse
• ​Boss 1986 Protostellar formation in rotating interstellar clouds. V - Nonisothermal collapse and fragmentation
• ​Boss 1987 Protostellar formation in rotating interstellar clouds. VI - Nonuniform initial conditions
• ​Boss 1988 Protostellar formation in rotating interstellar clouds. VII - Opacity and fragmentation
• ​Boss 1989 Protostellar formation in rotating interstellar clouds. VIII - Inner core formation
• ​Boss 1993 Collapse and fragmentation of molecular cloud cores. I - Moderately centrally condensed cores
• ​Boss 1995 Collapse and fragmentation of molecular cloud cores. 2: Collapse induced by stellar shock waves
• ​Boss 1995 Collapse and Fragmentation of Molecular Cloud Cores. III. Initial Differential Rotation
• ​Boss 1996 Collapse and Fragmentation of Molecular Cloud Cores. IV. Oblate Clouds and Small Cluster Formation
• ​Boss 1997 Collapse and Fragmentation of Molecular Cloud Cores. V. Loss of Magnetic Field Support
• ​Boss 1999 Collapse and Fragmentation of Molecular Cloud Cores. VI. Slowly Rotating Magnetic Clouds
• ​Boss 2002 Collapse and Fragmentation of Molecular Cloud Cores. VII. Magnetic Fields and Multiple Protostar Formation
• ​Boss 2005 Collapse and Fragmentation of Molecular Cloud Cores. VIII. Magnetically Supported Infinite Sheets
• ​Boss 2007 Collapse and Fragmentation of Molecular Cloud Cores. IX. Magnetic Braking of Initially Filamentary Clouds
• ​Cho & Kim 2011
  • 512³ Isothermal MHD fixed grid
  • beta=.1
  • J=4 (l_box/l_jeans)
  • M=10
  • Power law tail
  • Line-width size relation
• ​Cohn 1980 Late core collapse in star clusters and the gravothermal instability
• ​Ciardi & Hennebelle 2010
• ​Clark et al 2011 Gravitational Fragmentation in Turbulent Primordial Gas and the Initial Mass Function of Population III Stars
• ​Clark and Bonnell 2005
• ​Collins et al 2011
  • ENZO 128³+4 = 2048³; 10pc → 1000 AU; MHD Isothermal 10K; n=300/cc; B=.6+-2.7 microG (no AD) (supercritical)
  • power law tail for density (1.64) and B (2.74)
  • B = rho^.48
  • sigma = rho^.25 for cores
  • CMF = 2.1+-.6
• ​Elmegreen 2002 Star Formation from Galaxies to Globules
• ​Falgarone 1992 The small-scale density and velocity structure of quiescent molecular clouds
• ​Federrath et al 2010 Modeling Collapse and Accretion in Turbulent Gas Clouds: Implementation and Comparison of Sink Particles in AMR and SPH
• ​Federrath et al 2010 Comparing the statistics of interstellar turbulence in simulations and observations. Solenoidal versus compressive turbulence forcing
• ​Fiedler & Mouschovias 1992 Ambipolar diffusion and star formation: Formation and contraction of axisymmetric cloud cores. I - Formulation of the problem and method of solution
• ​Fiedler & Mouschovias 1993 Ambipolar Diffusion and Star Formation: Formation and Contraction of Axisymmetric Cloud Cores. II. Results
• ​Foster & Chevalier 1993 Gravitational Collapse of an Isothermal Sphere
• ​Furesz et al. 2008 Kinematic Structure of the Orion Nebula Cluster and its Surroundings
• ​Galli & Shu 1993 Collapse of Magnetized Molecular Cloud Cores. I. Semianalytical Solution
• ​Galli & Shu 1993 Collapse of Magnetized Molecular Cloud Cores. II. Numerical Results
• ​Gammie 1996 Linear Theory of Magnetized, Viscous, Self-gravitating Gas Disks
• ​Gammie & Ostriker 1996 Can Nonlinear Hydromagnetic Waves Support a Self-gravitating Cloud?
• ​Glover & Mac Low 2007 Simulating the Formation of Molecular Clouds. I. Slow Formation by Gravitational Collapse from Static Initial Conditions
• ​Glover & Mac Low 2007 Simulating the Formation of Molecular Clouds. II. Rapid Formation from Turbulent Initial Conditions* ​Goodman et al. 2009
• ​Goodwin et al. 2004 Simulating star formation in molecular cloud cores. I. The influence of low levels of turbulence on fragmentation and multiplicity
• ​Goodwin et al. 2004 Simulating star formation in molecular cores. II. The effects of different levels of turbulence
• ​Hartmann et al. 2001 Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood
• ​Heitsch et al 2000
• ​Heitsch et al 2001
• ​Heitsch et al 2005 Formation of Structure in Molecular Clouds: A Case Study
• ​Heitsch et al 2006 The Birth of Molecular Clouds: Formation of Atomic Precursors in Colliding Flows
• ​Heitsch et al 2008
• ​Hennebelle & Perault 2000 Dynamical condensation in a magnetized and thermally bistable flow. Application to interstellar cirrus
• ​Hennebelle et al. 2003 Protostellar collapse induced by compression
• ​Hennebelle et al. 2004 Protostellar collapse induced by compression - II. Rotation and fragmentation
• ​Hennebelle et al 2007 Diffuse interstellar medium and the formation of molecular clouds
• ​Heitsch & Hartmann 2008 Rapid Molecular Cloud and Star Formation: Mechanisms and Movies
• ​Hennebelle et al. 2008 From the warm magnetized atomic medium to molecular clouds
• ​hennebelle & Chabrier 2008 Analytical Theory for the Initial Mass Function: CO Clumps and Prestellar Cores
• ​Hennebelle & Chabrier 2009 Analytical Theory for the Initial Mass Function. II. Properties of the Flow
• ​Heyer et al. 2009
• ​Klessen et al 1998 Fragmentation of Molecular Clouds: The Initial Phase of a Stellar Cluster
• ​Klessen 2001
• ​Klessen et al 2000
• ​Klessen et al 2000
• ​Kritsuk et al 2011
  • ENZO 512³+5x2=524,288³; 5pc → 2 AU; Isothermal 10K; n=500/cc
  • Power law tail to density pdf
• ​Li et al 2004
• ​McKee Ostriker 2007
• ​Nakamura & Li 2008
  • 128³ isothermal MHD with AD and feedback 2.4 pc → .02 pc
  • B=15 microG (beta=1/24) subcritical
• ​Offner et al 2008
  • 1100/cc 10K
• ​Offner et al. 2008
• ​Offner et al 2009
• ​Ossenkopf 2001
• ​Shu 77
• ​Shu & Lizano 1989
• ​Tereby, Shu, & Cassen 1984
• ​Truelove 1997
• ​Truelove et al. 1998
• ​Vazques-Semadeni et al 2003 A Holistic Scenario of Turbulent Molecular Cloud Evolution and Control of the Star Formation Efficiency: First Tests

• ​Vazques-Semadeni et al. 2003 The Origin of Molecular Cloud Turbulence and its Role on Determining the Star Formation Efficiency

• ​Vazques-Semadeni et al 2006
• ​Vazques-Semadeni et al 2007
• ​Wang et al 2010