Other
Scientific paper
Apr 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...279..621m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 279, April 15, 1984, p. 621-632.
Other
127
Gravitational Collapse, Interstellar Matter, Molecular Clouds, Rotating Matter, Stellar Evolution, Fragmentation, Isothermal Processes, Space Density, Thermodynamic Equilibrium
Scientific paper
Isothermal collapse of a rotating interstellar cloud is computed three dimensionally with a so-called smoothed particle method. Initial clouds are rigidly rotating homogeneous spheres with small density fluctuations. To find a condition for fragmentation of a cloud, the authors test a wide range of initial conditions in the α0 - β0 plane, where α0 and β0 are the initial ratios of thermal and rotational energies to gravitational energy, respectively. The characteristics of collapse and fragmentation are determined essentially by the product α0β0. For α0β0 ⪆ 0.20, a cloud does not shrink appreciably and oscillates about an equilibrium configuration which is not very flattened. For α0β0 ⪉ 0.20, the inner part of a cloud contracts greatly to form a flattened disklike configuration. A cloud with α0β0 ⪉ 0.12 fragments and forms a multiple system, the multiplicitiy being larger for a cloud with smaller α0β0.
Hayashi Chuichiro
Miyama Shoken M.
Narita Shinji
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