Equilibrium and secular instability of rapidly rotating stars

Journal Article · Tue May 15 04:00:00 EDT 1979 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157079· OSTI ID:6250106

Clement, M J

Rotating main-sequence models in the mass range 1.5--30 M/sub sun/ have been computed with a two-dimensional relaxation technique. An analysis which incorporates a new criterion for marginal secular instability shows that differentially rotating stars reach the point of bifurcation at kinetic energies as much as 30% lower than those predicted by the tensor virial method.

• Research Organization: David Dunlap Observatory, University of Toronto
• OSTI ID: 6250106
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 230:1; 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
ATMOSPHERES
BOUNDARY CONDITIONS
CONVECTION
EQUILIBRIUM
INSTABILITY
MAIN SEQUENCE STARS
MATHEMATICAL MODELS
MOTION
ROTATION
STAR MODELS
STARS
STELLAR ATMOSPHERES