Low Mass Star Formation: Cold Dense Core Structure, Support, and Evolution.

Details Low Mass Star Formation: Cold Dense Core Structure, Support, and Evolution. Low Mass Star Formation: Cold Dense Core Structure, Support, and Evolution.

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21335603s&link_type=abstract

American Astronomical Society, AAS Meeting #213, #356.03; Bulletin of the American Astronomical Society, Vol. 41, p.498

Astronomy and Astrophysics

Astronomy

Scientific paper

Low-mass stars form in cold cloud cores; therefore, these cores represent the ideal -- and perhaps the only -- places to study effectively the initial conditions of star formation. Isolated cores are of particular interest because they are less affected by factors that can complicate the analysis, such as background and foreground emission from unassociated material, and external pressure and turbulence present in inter-core material, to name a few. We present Spitzer observations of four dense cores, complemented by molecular line observations. We use observations made with MIPS and IRAC of spatially resolved absorption features, termed shadows, caused by the cold dense core material, to derive the density structure. With molecular line observations we constrain the contributions of turbulent and thermal support. We highlight the observation of a 70 micron shadow in the starless core L429. This core is very likely to be prestellar, i.e., collapsing to form a star. We also present observations of an 8 micron shadow near B335, a globule known to contain a very young Class 0 protostar. The B335 shadow reveals that the dense core structure is organized into a flattened molecular core, with a spatial extent of about 10000 AU in diameter and with the same orientation as the circumstellar disk (about 100 to 200 AU in diameter). I will discuss these observations and place our sample of cores in an evolutionary context.

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