Nonadiabatic analysis of nonradial modes of stellar oscillation in the presence of slow rotation

Journal Article · Wed Dec 01 04:00:00 EST 1982 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160509· OSTI ID:5705421

Carroll, B W; Hansen, C J

The linearized equations governing nonadiabatic, nonradial pulsations of a slowly but uniformly rotating star have been derived. A large number of numerical examples are presented for near main sequence evolution of a 12 M/sub sun/ star. All modes with l = 2 and 3 and with periods between two and 15 hours were examined for this sequence. Other masses and values of l were studied, but to a lesser extent. For all modes and sequences studied it was found that slow, uniform rotation increases the pulsation frequency (as observed from an inertial frame) of prograde modes (m<0), and conversely for retrograde modes. The effect of rotation on stability is not as clear-cut. On the main sequence it enhances the stability of retrograde modes and makes prograde modes less stable. As evolution progresses, this distinction becomes less strong. Possible implications for ..beta.. Cephei and line profile variables are discussed.

• Research Organization: Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards; and the Department of Physics and Astro-geophysics, University of Colorado
• OSTI ID: 5705421
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 263:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics &amp; Cosmology-- Stars &amp; Quasi-Stellar
Radio &amp; X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
DIFFERENTIAL EQUATIONS
EQUATIONS
EQUATIONS OF MOTION
MAIN SEQUENCE STARS
MATHEMATICAL MODELS
MOTION
NUMERICAL SOLUTION
OSCILLATION MODES
OSCILLATIONS
PARTIAL DIFFERENTIAL EQUATIONS
ROTATION
STAR EVOLUTION
STAR MODELS
STARS
WAVE PROPAGATION