Protostellar formation in rotating interstellar clouds. IV Nonisothermal collapse

Details Protostellar formation in rotating interstellar clouds. IV Nonisothermal collapse Protostellar formation in rotating interstellar clouds. IV Nonisothermal collapse

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...277..768b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 15, 1984, p. 768-782. NASA-supported research.

Other

46

Astronomical Models, Gravitational Collapse, Interstellar Matter, Protostars, Rotating Matter, Stellar Evolution, Binary Stars, Eddington Approximation, Hydrodynamics, Nebulae, Radiative Transfer, Thermodynamics

Scientific paper

Radiative transfer in the Eddington approximation is included in a multidimensional, self-gravitational, hydrodynamical computer code. Details of the numerical solution and thermodynamic relations are given. Comparison calculations with previous spherically symmetrical models of protostellar collapse are used to validate the basic approach and the artifices which allow the explicit hydrodynamics code to follow the accretion of gas onto a quasi-equilibrium core. A series of axisymmetric models is used to investigate the importance of rotation in collapsing clouds, as the initial amount of angular momentum is lowered, with an emphasis on the possible formation of rings. Rings readily form even in the nonisothermal regime except for very low initial angular momenta; even these clouds may experience ring formation prior to reaching stellar densities. The models imply that other effects (such as gravitational torques or turbulent viscosity) may be necesary to avoid binary formation and thus result in a presolar nebula consistent with the assumptions of either Safronov or Cameron.

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