The formation phase of the solar nebula

Details The formation phase of the solar nebula The formation phase of the solar nebula

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...355..651b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 355, June 1, 1990, p. 651-660. Research supported by NASA.

Astronomy and Astrophysics

Astrophysics

62

Gravitational Collapse, Star Formation, Sun, Angular Momentum, Infrared Spectra, Protostars, Radiation Transport, Stellar Envelopes, Stellar Mass

Scientific paper

Hydrodynamical calculations of the collapse of an axisymmetric, rotating protostellar cloud, with radiation transport and without magnetic fields, are presented. The collapse is assumed to start from a centrally condensed sphere of radius 5 x 10 to the 15th cm, a mean density of 4 x 10 to the -15th g/cu cm, a total mass of 1 solar mass, and a total angular momentum of 10 to the 53rd g sq cm per sec. The numerical grid is chosen to resolve the region of disk formation between 1 and 60 AU from the center. Frequency-dependent radiative transfer calculations show how the emergent spectrum of the structure depends upon viewing angle with respect to the rotation axis and how the observed isophotal contours should depend on wavelength and viewing angle. The central part of the protostar, interior to 1 AU, is not resolved numerically but is modeled approximately. At the end of the calculation, this region is found to have a mass of 0.6 solar mass and a ratio of rotational to gravitational energy of about 0.4, sufficiently large to be unstable to nonaxisymmetric perturbations. Although the disk is gravitationally stable according to the local Toomre criterion, the nonaxisymmetric structure in the center is likely to lead to angular momentum transport.

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