Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....85..295s&link_type=abstract
Astronomy and Astrophysics, vol. 85, no. 3, May 1980, p. 295-301.
Astronomy and Astrophysics
Astrophysics
33
Binary Stars, Stellar Mass Accretion, Thermal Stability, White Dwarf Stars, Oscillations, Planetary Nebulae, Stellar Envelopes, Stellar Models
Scientific paper
Thermal and vibrational stabilities of accreting white dwarfs with steady-state nuclear burning were considered, assuming spherically symmetric accretion of the hydrogen-rich matter and using linear stability analysis. Almost all models with solar masses of 0.2-1.39 were found to be unstable in some way. The type of instability expected to dominate is given as a function of the accretion rate. For most accretion rates it is the thermal instability. Oscillation periods are given for the models in which the vibrational instability is the most violent one. These periods are of the order of seconds or minutes. It is expected that this stability analysis may suggest the cause of the variabilities of the hot components of some symbiotic stars, for a wide range of the accretion rates. In this case the proposed models may serve as the initial conditions for evolutionary computations. The results predict that short-period oscillations should be observed in some hot nuclei of planetary nebulae.
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