Equilibria of rotating, isothermal clouds. I. Method of solution

Journal Article · Sun May 01 04:00:00 EDT 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160941· OSTI ID:5832748

Stahler, S W

In an effort to resolve the current controversy in dynamical models of rotating protostellar collapse, a detailed study has been made of the axisymmetric equilibrium configurations for differentially rotating, isothermal clouds. In this paper, the physical assumptions underlying the calculation are stated and the numerical technique outlined. The clouds are assumed to have the angular momentum distribution of rigidly rotating, uniform-density spheres of the same mass. Magnetic and viscous effects are neglected. The computational method is designed to handle highly flattened structures, should they arise, and to yield numerical values of the density with a maximum local error of order 1/N/sup 2//sub X/, where N/sub X/ is the number of zones covering the cloud's equatorial radius. A preliminary calculation, with N/sub X/ = 10, of nonrotating spherical equilibria reproduces the Lane--Emden result to within the desired accuracy. Errors in global properties, as measured by a test of the virial theorem, are about a factor of 10 lower than the maximum local error.

• Research Organization: Center for Radiophysics and Space Research, Cornell University
• OSTI ID: 5832748
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 268:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
FLUID MECHANICS
GRAVITATION
HYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
MOTION
NEBULAE
NUMERICAL SOLUTION
ROTATION
STAR ACCRETION
STAR EVOLUTION
VIRIAL THEOREM