On the evolution of gravitationally unstable protostellar disks

Details On the evolution of gravitationally unstable protostellar disks On the evolution of gravitationally unstable protostellar disks

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...382..530t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 382, Dec. 1, 1991, p. 530-543. Research supported by NASA.

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70

Gravitational Collapse, Many Body Problem, Protostars, Star Formation, Stellar Evolution, Angular Momentum, Astronomical Models, Computational Astrophysics, Interstellar Matter, Stellar Envelopes, T Tauri Stars

Scientific paper

2D, N-body simulations of the nonlinear development of long-wavelength instabilities predicted to occur early in the formation stage of protostellar disks forming single stars are presented under conditions of controlled energy loss. It is found that the thermodynamics and long-term evolution of gravitationally unstable disks are intimately coupled: the global evolution rate is linearly proportional to the rate at which dissipated energy reaches and escapes from the surfaces of the disk. An upper limit is obtained to the rate at which energy is lost if it is assumed that the disk maintains vertical isothermality.

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