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Undergoing spherically symmetric steady-state accretion stability of white dwarfs

Journal Article:

Abstract

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 masses 0.2 M(sun) - 1.39 M(sun) 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. We expect that our 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 our 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.
Authors:
Sienkiewicz, R [1] 
  1. Polska Akademia Nauk, Warsaw. N. Copernicus Astronomical Center
Publication Date:
Jan 01, 1980
Product Type:
Journal Article
Reference Number:
AIX-11-542677; EDB-81-029007
Resource Relation:
Journal Name: Astron. Astrophys.; (Germany, Federal Republic of); Journal Volume: 85:3
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; WHITE DWARF STARS; STAR ACCRETION; BOUNDARY CONDITIONS; EXCITATION; INSTABILITY; LUMINOSITY; OSCILLATIONS; STABILITY; STAR BURNING; STAR MODELS; STEADY-STATE CONDITIONS; TEMPERATURE DEPENDENCE; DWARF STARS; ENERGY-LEVEL TRANSITIONS; MATHEMATICAL MODELS; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; STAR EVOLUTION; STARS; 640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
OSTI ID:
6982157
Country of Origin:
Germany
Language:
English
Other Identifying Numbers:
Journal ID: CODEN: AAEJA
Submitting Site:
INIS
Size:
Pages: 295-301
Announcement Date:

Journal Article:

Citation Formats

Sienkiewicz, R. Undergoing spherically symmetric steady-state accretion stability of white dwarfs. Germany: N. p., 1980. Web.
Sienkiewicz, R. Undergoing spherically symmetric steady-state accretion stability of white dwarfs. Germany.
Sienkiewicz, R. 1980. "Undergoing spherically symmetric steady-state accretion stability of white dwarfs." Germany.
@misc{etde_6982157,
title = {Undergoing spherically symmetric steady-state accretion stability of white dwarfs}
author = {Sienkiewicz, R}
abstractNote = {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 masses 0.2 M(sun) - 1.39 M(sun) 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. We expect that our 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 our 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.}
journal = {Astron. Astrophys.; (Germany, Federal Republic of)}
volume = {85:3}
journal type = {AC}
place = {Germany}
year = {1980}
month = {Jan}
}