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Origin of Very-Short Orbital-Period Binary Systems

Published online by Cambridge University Press:  12 April 2016

Shigeki Miyaji
Shigeki Miyaji*
Affiliation:
Department of Natural History, College of Arts and Sciences, Chiba University, Chiba 260, Japan

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Recent observations of four close binaries have established that there is a group of very-short orbital-period (VSOP) binaries whose orbital periods are less than 60 minutes. The VSOP binaries consist of both x-ray close binaries (4U1626-67; Middleditch et al. 1981 and 4U1916 -0.5; White and Swank 1982) and cataclysmic variables (AM CVn; Faulkner et al. 1972 and G61-29; Nather et al. 1981). Their orbital periods are too short to have a main-sequence companion. However, four binaries, none of them belongs to any globular cluster, are too abundant to be explained by capturing mechanism of a white dwarf. Therefore it seemed to be worth to present an evolutionary scenario from an original binary system which can be applied for all of VSOP binaries.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 72: Cataclysmic Variables and Related Objects , 1983 , pp. 263 - 267
Copyright
Copyright © Reidel 1983

References

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