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Be Stars in Roche-Lobe Interacting Binaries

Published online by Cambridge University Press:  12 April 2016

A.E. Tarasov
A.E. Tarasov*
Affiliation:
Crimean Astrophysical Observatory, Nauchny, Crimea, 98908Ukraine

Abstract

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Different types of massive interacting binaries with Be components are discussed. Due to mass exchange, Be stars in these systems have some peculiar characteristics. Often it is even difficult to find traces of the Be star and/or mass-losing star in the optical region of the spectrum. Using the value of the orbital period as a primary parameter, it is possible to divide all massive interacting binaries into two large groups: short-period or classical Algols and long-period binaries. The last group includes a number of very active mass transfer systems named as W Serpentis. There is also a small group of double systems whose stars do not fill their Roche lobes but have emission lines in the spectrum. Properties of their spectral variability are discussed. Analysis of each group lets us find different behaviours in mass exchange that depend on the size of their Roche lobes.

Type
7. Interacting Binaries
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 644 - 655
Copyright
Copyright © Astronomical Society of the Pacific 2000

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