Star formation in colliding gas flows

Details Star formation in colliding gas flows Star formation in colliding gas flows

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...305..309h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 305, June 1, 1986, p. 309-332. DOE-supported research.

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Computation

86

Astronomical Models, Gas Flow, Molecular Clouds, Stellar Evolution, Computational Astrophysics, Flow Velocity, Fragmentation, Gas Density, Gravitation, Hydrodynamic Equations

Scientific paper

Gas flows colliding within molecular clouds produce regions of compressed gas and dust that are hydrodynamically unstable. Fragmentation of the compressed region produces clumps in the mass range 0.01 ≤ m ≤ 5.0 M_sun;, in time tb ≈ 5x1012s. Gravitational instability of the fragment distribution occurs on the time scale tc ≈ 1013s. The gravitational attraction of the clumps and the disk material can form protostars in the mass range 1.0 ≤ mf ≤ 65.0 M_sun;. The conditions for dynamical fragmentation to occur do not require that the overall molecular cloud be Jeans unstable, or even that it be collapsing; there must only be a source for the kinetic energy of the gas flows that interact. These results support the conclusion that the star formation process in molecular clouds can be triggered by high-velocity gas-flow interactions within molecular clouds.

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