Structure formation via the self-gravity interfacial instability

Details Structure formation via the self-gravity interfacial instability Structure formation via the self-gravity interfacial instability

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.7006h&link_type=abstract

American Astronomical Society Meeting 203, #70.06; Bulletin of the American Astronomical Society, Vol. 35, p.1317

Astronomy and Astrophysics

Astronomy

Scientific paper

Interfacial instabilities (such as Rayleigh-Taylor or Kelvin-Helmholtz) are believed to play significant roles in shaping molecular clouds and giving rise to star forming regions. Recent studies (Hunter, Whitaker,and Lovelace ApJ 482, 1997; Hueckstaedt and Hunter MNRAS 327, 2001) have shown that self-gravity causes crenulations along a density interface to grow as the system seeks a lower energy state. The self-gravity interfacial instability (SGI) persists for wavelengths less that the Jean's length and has a timescale on the order of the freefall time. We discuss the SGI and its application toward molecular cloud morphology.

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