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Non-Conservative Mass Exchange and Origin of X-Ray Close Binaries

Published online by Cambridge University Press:  14 August 2015

Daiichiro Sugimoto  and
Shigeki Miyaji
Daiichiro Sugimoto
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo, Tokyo 153, Japan
Shigeki Miyaji
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo, Tokyo 153, Japan

Extract

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Recently, masses of component stars have been determined for many X-ray close binaries (XCBS). For relatively well determined sources the masses of X-ray components are plotted against the masses of their optical components in Figure 1 and their orbital periods are summarized in Table 1 (Cowley 1977; Bradt, Doxsey, and Jernigan 1979; Wheeler 1978; and references quoted therein). Cowley (1977) prepared a table and noticed that there are two distinct types of XCBS. The Type I XCBS consists of an X-ray star and an early type star more massive than about 12 M⊙. On the contrary, the Type II XCBS consists of an X-ray star and a star less massive than about 2 M⊙. As seen in Figure 1, there is not any distinct intermediate type for which the mass of the optical component lies in the range of about 2-12 M⊙. The aim of the present paper lies in interpreting the origin of these types of XCBS on the bases of the conditions for the formation of a neutron star and of mass exchange in close binary systems.

Type
VI. X-Ray Binaries
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 323 - 327
Copyright
Copyright © Reidel 1980 

References

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