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Fragmentation in a rotating protostar - A comparison of two three-dimensional computer codes
Boss, A. P.; Bodenheimer, P.
AA(California, University, Santa Barbara, Calif.), AB(NASA, Ames Research Center, Space Science Div., Moffett Field; Lick Observatory, Santa Cruz, Calif.)
Astrophysical Journal, Part 1, vol. 234, Nov. 15, 1979, p. 289-295. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Computer Programs, Gravitational Collapse, Hydrodynamics, Mathematical Models, Protostars, Stellar Evolution, Binary Stars, Fragmentation, Pressure Effects, Stellar Gravitation, Stellar Rotation
Bibliographic Code:


The collapse of an isothermal protostellar cloud with pressure, gravity, and rotation included is followed with two independent computer codes. For the initial condition, a nonaxisymmetric perturbation of mode m = 2 and 50% amplitude is introduced into a cloud of 1 solar mass with a mean density of 1.44 x 10 to the -17g/cu cm and a uniform angular velocity of 1.6 x 10 to the -12 rad/sec. The collapse is followed through an increase in density of over four orders of magnitude to the point where a binary protostar forms. The agreement between the results of the two calculations is good.

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Database: Astronomy
arXiv e-prints