Equilibrium models of self-gravitating inviscid disks resulting from the collapse of rotating clouds

Details Equilibrium models of self-gravitating inviscid disks resulting from the collapse of rotating clouds Equilibrium models of self-gravitating inviscid disks resulting from the collapse of rotating clouds

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...351..206s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 351, March 1, 1990, p. 206-221.

Statistics

Computation

13

Astronomical Models, Gravitational Collapse, Rotating Matter, Star Formation, Angular Momentum, Computational Astrophysics, Density Distribution, Integral Equations

Scientific paper

A method is presented for the construction of velocity and surface density profiles of infinitely thin, self-gravitating disks formed from the collapse of spherical clouds, under the condition that the angular momentum of each material parcel is conserved. Results are presented for initially uniformly rotating clouds with density distributions varying as R exp -n and n = 0, 1, 2. The resulting disk surface density distributions are well represented by power laws in the cylindrical radius over most of their extent. The form of the zeroth-order approximation provides a useful representation of the final surface density function near the center for all three cases, and for n = 2 this result holds throughout the disk. This result is not generally true for the velocity functions, however.

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