Computer simulations of the formation of massive protostars

Details Computer simulations of the formation of massive protostars Computer simulations of the formation of massive protostars

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256..291p&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 2, May 15, 1992, p. 291-299.

Statistics

Computation

17

Accretion Disks, Computerized Simulation, Interstellar Gas, Molecular Clouds, Protostars, Shock Waves, Star Formation, Compressed Gas, Computational Astrophysics, Particle Collisions, Stellar Evolution, Supersonic Speed

Scientific paper

Attention is given to computer simulations of massive protostar formation which show that in regions of supersonic turbulence such as giant molecular clouds, protostars readily and rapidly condense out of the dense layers which form where two turbulent elements collide at high relative speed. The resulting protostars are rotationally supported disks with well-defined accretion surfaces, masses between 1 and 20 solar masses, diameters in the range 100-400 AU, and densities above 10 exp 12 H2/cu cm, i.e., 10 exp 10 times the initial gas density. The time-scale for formation of these protostellar disks turns out to be shorter than the free-fall time-scale in the initial clouds.

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