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Instability of g-Mode Oscillations in White Dwarf Stars
Published online by Cambridge University Press: 12 April 2016
Abstract
A white dwarf model with M=.6 M⊙, Te=12000K, and L=1.2×1031 erg sec-1 provided by A.N. Cox has been tested for linear stability of radial oscillations. The radial mode instability first reported for this model by Cox, et. al (1979) has been confirmed. The growth rates obtained are comparable to the rates found by Cox. A sequence of ℓ=2 g-modes has also been found to be unstable. The e-folding times range from around 1011 periods for a 137 second mode (1 radial node) to less than 100 periods for a 629 second mode (17 nodes). It is likely that the latter rate is too high because the eigenfunction has been forced to vanish at the non-zero inner radius of the model, at which the Brunt-Väisäla frequency is barely less than the mode frequency.
- Type
- Colloquium Session VI
- Information
- International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 388 - 391
- Copyright
- Copyright © The University of Rochester 1979
References
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