Computer Science
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..369f&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
1
Scientific paper
We show three-dimensional numerical simulations in which stars are formed sequentially in a filamentary molecular cloud by dynamical influence of H II region. The H II region is distant from the filamentary cloud at the initial stage. As it expands, it interacts with the filamentary cloud. The cloud is pinched and separated into two. Subsequently, the gravitational instability is induced to form two cores of the first-generation along the filament axis. The separation of the two cores is several times larger than the filament diameter. It is comparable to the wavelength of the fastest growing fragmentation mode. The first-generation cores become isolated and filamentary clouds shorten to widen the gap. New cores of second-generation form at the edges of the shortened filamentary clouds. This core formation is recursive and our model shows sequential star formation induced by an expanding H II region. The age difference is several times of the dynamical scale between the first- and second- generation cores. This sequential star formation is similar to that observed in the filamentary cloud associated with the H II region NGC2024. Our first-generation cores correspond to FIR 4 and FIR 5 while the second-generation cores to FIR 3 and FIR 6.
Fukuda Naoya
Hanawa Tomoyuki
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