Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976afz....12..521t&link_type=abstract
Astrofizika, vol. 12, Aug. 1976, p. 521-530. In Russian.
Astronomy and Astrophysics
Astronomy
33
Binary Stars, Dwarf Stars, Giant Stars, Stellar Evolution, Hot Stars, Stellar Envelopes, Stellar Mass Ejection, Symbiosis
Scientific paper
Properties of symbiotic stars are examined on the basis of a model consisting of a red giant and a hot dwarf surrounded by a common nebulosity in an attempt to determine the evolutionary stage of such systems. It is shown that the hot components should be either helium stars in the stage of core helium burning or carbon-oxygen dwarfs with thin hydrogen-helium shells, while the cold components should be red giants losing mass at a rate of about one hundred-thousandth to one millionth of a solar mass per year over a period of 100,000 to 1 million years. The possibility of forming symbiotic stars in the course of binary-system evolution is investigated. It is concluded that these systems may form in three ways: from widely separated pairs by either envelope loss from an initially more massive system due to continuous outflow or mass ejection as a consequence of a dynamic instability during the red giant stage and from closer pairs by mass exchange between components. The instability leading to flares of symbiotic stars is briefly considered.
Iungelson L. R.
Tutukov Aleksandr V.
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