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Symbiotic stars - a binary model with super-critical accretion

Abstract

The structure of symbiotic variables is discussed in terms of a binary model. Disc accretion by a main sequence star or white dwarf at rates close to the Eddington limit produces an ultraviolet continuum source near the accreting star surface. This generates a variable, radiatively-driven, out-flowing wind. The wind is optically thick and the disc luminosity is absorbed and scattered and thus degraded into the optical region. Variations in the rate of mass loss in the wind lead to optical eruptions through shifts in the position of, and conditions in, the last scattering surface. The behaviour of Z And determined by Boyarchuk is shown to be in agreement with such a model. The conditions in the out-flowing wind are discussed. Limits on the mass loss rate are derived from conditions at the surface of the accreting star. It is suggested that variable out-flow in the wind is generated by fluctuations in disc luminosity produced by changes in the giant companions rate of mass transfer. The relation between symbiotic variables and classical and dwarf novae is discussed.
Authors:
Bath, G T [1] 
  1. National Radio Astronomy Observatory, Charlottesville, Va. (USA)
Publication Date:
Jan 01, 1977
Product Type:
Journal Article
Reference Number:
AIX-08-300424; EDB-77-083968
Resource Relation:
Journal Name: Mon. Not. R. Astron. Soc.; (United Kingdom); Journal Volume: 178:1
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; BINARY STARS; STAR ACCRETION; STAR MODELS; MAIN SEQUENCE STARS; VARIABLE STARS; WHITE DWARF STARS; BOUNDARY CONDITIONS; LUMINOSITY; MASS TRANSFER; SCATTERING; STELLAR WINDS; ULTRAVIOLET RADIATION; VARIATIONS; VISIBLE RADIATION; DWARF STARS; ELECTROMAGNETIC RADIATION; MATHEMATICAL MODELS; OPTICAL PROPERTIES; PHYSICAL PROPERTIES; RADIATIONS; STAR EVOLUTION; STARS; 640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
OSTI ID:
7304830
Country of Origin:
United Kingdom
Language:
English
Other Identifying Numbers:
Journal ID: CODEN: MNRAA
Submitting Site:
INIS
Size:
Pages: 203-217
Announcement Date:
May 01, 1977

Citation Formats

Bath, G T. Symbiotic stars - a binary model with super-critical accretion. United Kingdom: N. p., 1977. Web.
Bath, G T. Symbiotic stars - a binary model with super-critical accretion. United Kingdom.
Bath, G T. 1977. "Symbiotic stars - a binary model with super-critical accretion." United Kingdom.
@misc{etde_7304830,
title = {Symbiotic stars - a binary model with super-critical accretion}
author = {Bath, G T}
abstractNote = {The structure of symbiotic variables is discussed in terms of a binary model. Disc accretion by a main sequence star or white dwarf at rates close to the Eddington limit produces an ultraviolet continuum source near the accreting star surface. This generates a variable, radiatively-driven, out-flowing wind. The wind is optically thick and the disc luminosity is absorbed and scattered and thus degraded into the optical region. Variations in the rate of mass loss in the wind lead to optical eruptions through shifts in the position of, and conditions in, the last scattering surface. The behaviour of Z And determined by Boyarchuk is shown to be in agreement with such a model. The conditions in the out-flowing wind are discussed. Limits on the mass loss rate are derived from conditions at the surface of the accreting star. It is suggested that variable out-flow in the wind is generated by fluctuations in disc luminosity produced by changes in the giant companions rate of mass transfer. The relation between symbiotic variables and classical and dwarf novae is discussed.}
journal = []
volume = {178:1}
journal type = {AC}
place = {United Kingdom}
year = {1977}
month = {Jan}
}