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Dense Cores and Their Environs

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. Difference in V C is small - usually less than the sound speed (see also Walsh & Myers 2004, 2007).

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Dense Cores and Their Environs

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  1. 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

  2. Difference in VC is small - usually less than the sound speed (see also Walsh & Myers 2004, 2007) Dynamics of Dense Cores in Perseus • IRAM 30m survey of ~100 dense cores in N2H+ (1-0) and C18O(2-1), plus whole cloud coverage in 13CO(1-0) (COMPLETE) N2H+ C18O Kirk, Johnstone, & Tafalla 2007

  3. 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

  4. Core Motion 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 velocity dispersion of lower density environment (from 13CO) Kirk, Johnstone, & Basu 2009

  5. 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!

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