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

• ​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
• ​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
• ​Goodman et al. 2009
• ​Heitsch et al 2001
• ​Heitsch et al 2000
• ​Heitsch et al 2008
• ​Hennebelle et al 2008
• ​Heyer et al. 2009
• ​Hennebelle & Chabrier 2008*
• ​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