Formation of Low Mass Stars in Turbulent Molecular Cloud Cores

Details Formation of Low Mass Stars in Turbulent Molecular Cloud Cores Formation of Low Mass Stars in Turbulent Molecular Cloud Cores

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..apr.b8003k&link_type=abstract

American Physical Society, April Meeting, 2004, May 1-4, 2004, Denver, Colorado April 2004, MEETING ID: APR04, abstract #B8.003

Physics

Scientific paper

The formation of Giant Molecular Clouds (GMCs) sets the stage for the formation of protostellar systems by the gravitational collapse of dense regions within the GMC that fragment into smaller core components that in turn condense into stars. Inherent in the difficulty in developing a theory of low mass star formation is that the gravitational collapse depends critically upon initial conditions within the cores which only recently have been known with sufficient accuracy to permit a realistic theoretical attack on the problem. A major goal of this research is to understand the nature and physical properties of the formation of binary and multiple stellar systems with typical low mass stars 0.2 to 3 solar masses. We use our powerful parallel adaptive mesh refinement (AMR) self-gravitational radiation hydrodynamics code to study gravitational collapse across many orders of magnitude in density. We present preliminary results for the investigation of turbulent molecular cloud cores as they evolve from larger scale turbulent clouds, and follow the collapse of high mass fragments as they interact with the radiation of the protostars forming at their centers. We show how previous calculations using SPH are significantly under-resolved and their failure to satisfy the minimum requirements of the Jeans Condition leads to false fragmentation.

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