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

Author

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  • Alyssa A. Goodman

    (Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
    Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA)

  • Erik W. Rosolowsky

    (Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA
    University of British Columbia, Okanagan, Kelowna, British Columbia V1V 1V7, Canada)

  • Michelle A. Borkin

    (Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
    Present address: School of Engineering and Applied Sciences, Harvard University, 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
    Brigham and Women’s Hospital, Harvard Medical School, Boston, Massachusetts 02115, USA)

  • Jens Kauffmann

    (Initiative in Innovative Computing at Harvard, Cambridge, Massachusetts 02138, USA
    Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA)

  • Jaime E. Pineda

    (Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA)

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.

Suggested Citation

  • Alyssa A. Goodman & Erik W. Rosolowsky & Michelle A. Borkin & Jonathan B. Foster & Michael Halle & Jens Kauffmann & Jaime E. Pineda, 2009. "A role for self-gravity at multiple length scales in the process of star formation," Nature, Nature, vol. 457(7225), pages 63-66, January.
    • Handle: RePEc:nat:nature:v:457:y:2009:i:7225:d:10.1038_nature07609
    DOI: 10.1038/nature07609
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