Linear, nonadiabatic analysis of nonradial oscillations of massive near main sequence stars

Details Linear, nonadiabatic analysis of nonradial oscillations of massive near main sequence stars Linear, nonadiabatic analysis of nonradial oscillations of massive near main sequence stars

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..549s&link_type=abstract

Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 549-559.

Computer Science

Numerical Analysis

76

Main Sequence Stars, Numerical Analysis, Oscillations, Pulsed Radiation, Stellar Mass, Variable Stars, Linear Equations, Opacity, Stellar Evolution, Stellar Models

Scientific paper

The equations for linear, nonadiabatic, nonradial oscillations have been solved for models with 7, 12, and 20 solar masses in the core-hydrogen burning and hydrogen exhaustion phases. Although the nonadiabatic periods are essentially the same as those of the corresponding adiabatic ones for those models investigated, the e-folding times for the oscillation amplitude are considerably different from the results of a quasi-adiabatic analysis, in particular for f and p modes. All the modes investigated are stable. However, the opacity bump near the He(+) ionization zone has a destabilizing influence on nonradial modes in the 7 solar-mass models about as strong as on purely radial oscillations. The effective temperatures of the 12 solar-mass and 20 solar-mass models are too high for the opacity bump mechanism to be effective as a destabilizing mechanism for nonradial modes. For the g(+) modes another driving zone exists in the intermediate-to-high temperature region.

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