Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...199..179d&link_type=abstract
Astrophysical Journal, vol. 199, July 1, 1975, pt. 1, p. 179-183. NASA-supported research
Astronomy and Astrophysics
Astronomy
28
Astronomical Models, Dynamic Stability, Stellar Mass, Stellar Rotation, White Dwarf Stars, Binary Stars, Degenerate Matter, Gravitational Waves, Mass Transfer, Secular Variations, Stellar Structure, X Ray Astronomy
Scientific paper
Models of nonmagnetic axisymmetric differentially rotating zero-temperature white dwarfs are constructed and tested for stability. Upper mass limits, beyond which models become secularly and dynamically unstable to growth of nonaxisymmetric perturbations, are found at 2.5 solar masses and 4.6 solar masses, respectively. The upper mass limit for secular stability is practically the same for the two angular momentum distributions considered. Crude growth rates due to gravitational radiation and degenerate-electron viscosity are calculated for the secularly unstable models. Except for a narrow parameter range, gravitational radiation is the dominant destabilizing mechanism. For masses between 3.5 and 4.6 solar masses, the secular instability grows on a time scale of about 10 to 1000 years; for masses exceeding about 4.6 solar masses, the dynamic instability grows on a time scale of seconds. Implications of these results for mass-transfer binary star systems and degenerate stellar cores are discussed.
No associations
LandOfFree
Upper mass limits for stable rotating white dwarfs does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Upper mass limits for stable rotating white dwarfs, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Upper mass limits for stable rotating white dwarfs will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1755096