A role for self-gravity at multiple length scales in the process of star formation

Alyssa A. Goodman (), Erik W. Rosolowsky, Michelle A. Borkin, Jonathan B. Foster, Michael Halle, Jens Kauffmann and Jaime E. Pineda
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Alyssa A. Goodman: Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
Erik W. Rosolowsky: Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA
Michelle A. Borkin: Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
Jonathan B. Foster: Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA
Michael Halle: Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
Jens Kauffmann: Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
Jaime E. Pineda: Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA

Nature, 2009, vol. 457, issue 7225, 63-66

Abstract: Self-gravity in star formation Stars and planets form from collapsed cores of dense molecular gas produced by the fragmentation of molecular clouds. Although self-gravity is known to be a major factor in the late stages of star formation, its importance at earlier times — and on larger length scales — is unclear. Goodman et al. report a new 'dendrogram' analysis of a previously obtained high-dynamic-range spectral-line map that reveals the hierarchical structure of gas inside the star-forming molecular cloud L1448. The analysis shows that self-gravity plays a significant role at all scales traced in the observations, though not in all regions. This is in qualitative agreement with models that favour 'turbulent fragmentation', although the amount of self-gravitating material found is lower than current models predict.

Date: 2009
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DOI: 10.1038/nature07609

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