Equilibria and evolutions of magnetized, rotating, isothermal clouds. I. Basic equations and numerical methods

Journal Article · Tue Mar 01 04:00:00 EST 1988 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/166082· OSTI ID:6995606

Tomisaka, K; Ikeuchi, S; Nakamura, T

It is shown that the equilibrium structure of a self-gravitating, magnetized, isothermal cloud with rotation can be solved by the self-consistent field method, like that employed in the pioneering work on a magnetized cloud without rotation by Mouschovious. Clouds are assumed to be axisymmetric and are embedded in a stationary external medium. The equilibrium problem is characterized by four free parameters; the central gas density, the total angular momentum, the total mass, and the magnetic flux. Two free functions, the distributions of specific angular momentum and mass within a cloud, should be given. These six quantities characterize each equilibrium model. Several numerical examples are shown. 13 references.

• Research Organization: Tokyo Astronomical Observatory, Mitaka (Japan); Kyoto Univ., (Japan)
• OSTI ID: 6995606
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 326; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
COSMIC GASES
DENSITY
DISTRIBUTION
EQUILIBRIUM
FLUID MECHANICS
FLUIDS
GASES
HYDRODYNAMICS
INTERSTELLAR SPACE
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MASS
MASS DISTRIBUTION
MATHEMATICAL MODELS
MECHANICS
MOTION
NEBULAE
NUMERICAL SOLUTION
PHYSICAL PROPERTIES
ROTATION
SELF-CONSISTENT FIELD
SPACE
SPATIAL DISTRIBUTION