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Angular-Momemtum Transfer by Nonradial Oscillations in Massive Main-Sequence Stars

Published online by Cambridge University Press:  12 April 2016

Umin Lee  and
Hideyuki Saio
Umin Lee
Affiliation:
Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, U.S.A.
Hideyuki Saio
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Sendai, Miyagi 980, Japan.

Extract

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Angular mementum distribution is one of the most important factors for stellar structutre and evolution. Among other mechanisms, angular momentum is transfered by non-axisymmetric oscillations (nonradial oscillations). In this mechanism the angular momentum is carried mainly by the Reynolds stress, which is proportional to the product between radial and azimuthal components of oscillation velocity; i.e., (Φ direction is the direction of rotation velocity). In the linear oscillation analysis, the phase difference between and is with A finite value of δ, which arises from excitation or damping of the oscillation, makes the time average of finite. Positive angular momentum is transfered from the driving zone to the damping zone by a prograde mode (Osaki 1986).

Type
III. Input physics for stellar structure
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 287 - 289
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Lee, U. 1988, MNRAS, 232, 711.CrossRefGoogle Scholar
Lee, U. & Saio, H. 1986, MNRAS, 221, 711.Google Scholar
Lee, U. & Saio, H. 1987, MNRAS, 225, 643.CrossRefGoogle Scholar
Lee, U. & Saio, H. 1990, ApJ, 360, 590.Google Scholar
Osaki, Y. 1986, PASP, 98, 32.CrossRefGoogle Scholar