Computer Science – Sound
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..141h&link_type=abstract
Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam
Computer Science
Sound
Scientific paper
We discuss dynamical collapse of a dense core with emphasis on the bar mode instability. Recent numerical simulations show that a dynamically collapsing core changes its form from sphere through disk to filament. The filament is much longer than the Jeans length and likely to be unstable against fragmentation. We discuss the mechanism of filament formation on the basis of linear stability analysis. According to our analysis, a dynamically collapsing gas sphere is unstable against the bar mode, i.e., a non-spherical density perturbation proportional to, Y 2 m(θ,ϕ) . The filament formation is due to the bar mode instability. The bar mode grows with the time, t , in proportion to ěrt t - t 0 ěrt -σ while the central density increases in proportion to (t - t 0 ) -2 . When the collapse is isothermal, the growth rate is σ = 0.354 . The growth rate is larger when the sound speed decreases with the increase in the density. This bar mode instability may lead to fragmentation in a core and may be related to binary formation.
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