Dense Cores and Their Environs Helen Kirk NSERC PDF with Doug Johnstone (HIA / UVic) Shantanu Basu (UWO) & Mario Tafalla (OAN, Spain) Dense Cores in Dark.

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Presentation transcript:

Dense Cores and Their Environs Helen Kirk NSERC PDF with Doug Johnstone (HIA / UVic) Shantanu Basu (UWO) & Mario Tafalla (OAN, Spain) Dense Cores in Dark Clouds 2009

Dynamics of Dense Cores in Perseus IRAM 30m survey of ~100 dense cores in N 2 H + (1-0) and C 18 O(2-1), plus whole cloud coverage in 13 CO(1-0) (COMPLETE) N2H+N2H+ C 18 O Difference in V C is small - usually less than the sound speed (see also Walsh & Myers 2004, 2007) Kirk, Johnstone, & Tafalla 2007

Comparison to Simulations (Ciolek & Basu 2006; Basu, Ciolek & Wurster 2009) Examined 20 thin sheet MHD simulations spanning  = 0.5 to 2 and M = 0 to 4 ‘observed’ to mimic Perseus observations  =0.5,M=1  =2.0,M=3

Core Motion velocity dispersion of lower density environment (from 13 CO) difference in centroid velocities Note: Other quantities in the simulations, such as the core linewidth, match observations well! Discrepancy may be due to periodic boundary conditions, different geometry, etc Kirk, Johnstone, & Basu 2009

Future Directions : Gould Belt Legacy Surveys The dynamical relationship between dense cores and their environment can constrain models of star formation Gould Belt Surveys (JCMT, Spitzer, Herschel) will soon be providing a wealth of data to base further dynamical surveys  effect of environment on core formation can be investigated!