Equilibria and evolutions of magnetized, rotating, isothermal clouds. II - the extreme case: nonrotating clouds

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

DOI:https://doi.org/10.1086/166923· OSTI ID:6494211

Tomisaka, K; Ikeuchi, S; Nakamura, T

Equilibrium solutions of magnetized nonrotating clouds in a static external medium were obtained for a wide ranges of parameters. Two different equilibrium states with the same mass but different central densities were obtained, and it is shown that the solution with lower central density is stable, while that with higher central density is unstable. Two possibilities for the initiation of star formation are suggested: (1) the mass of cloud exceeds M(cr) and (2) the cloud is compressed beyond the unstable equilibrium solution with higher central density. 23 references.

• Research Organization: Niigata Univ. (Japan); National Astronomical Observatory, Mitaka (Japan); Kyoto Univ. (Japan)
• OSTI ID: 6494211
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 335; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC GASES
DENSITY
DISTRIBUTION
FLUID MECHANICS
FLUIDS
GASES
HYDRODYNAMICS
INTERSTELLAR MAGNETIC FIELDS
INTERSTELLAR SPACE
ISOTHERMAL PROCESSES
MAGNETIC FIELD CONFIGURATIONS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MASS
MASS DISTRIBUTION
MECHANICS
MOTION
NEBULAE
PHYSICAL PROPERTIES
ROTATION
SPACE
SPATIAL DISTRIBUTION
STAR EVOLUTION