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Instability of g-mode oscillations in white dwarf starsA white dwarf model with M = 6 solar masses, Te = 12,000 K, and L = 1.2 x 10 to the 31st erg/sec provided by 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 10 to the 11th 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-Vaisala frequency is barely less than the mode frequency.
Document ID
19810032892
Document Type
Conference Proceedings
Authors
Keeley, D. A. (Science Applications, Inc. Palo Alto, Calif., United States)
Date Acquired
August 11, 2013
Publication Date
January 1, 1979
Subject Category
ASTROPHYSICS
Meeting Information
Annual Workshop on Novae, Dwarf Novae and Other Cataclysmic Variables
Funding Number(s)
CONTRACT_GRANT: NSG-7342
Distribution Limits
Public
Copyright
Other