THE AM CANUM-VENATICORUM STARS

被引:110
作者
WARNER, B
机构
[1] Department of Astronomy, University of Cape Town, Rondebosch
关键词
D O I
10.1007/BF00613240
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The photometric and spectroscopic properties of the six known AM CVn stars are reviewed. This gives support to the idea that they are helium-transferring double degenerate binaries with orbital periods in the range 1000-3000 s. The photometric variations arise predominantly from the same 'superhump' phenomenon that is seen in superoutbursts of the SU UMa subclass of H-rich cataclysmic variable stars. This enables tentative masses and mass ratios to be obtained for some of the AM CVn systems. An evolutionary scheme is proposed, linking the various behaviours of the AM CVn systems. AM CVn and EC15330-1403 are the equivalent of nova-like variables, with high mass transfer stable accretion discs. CR Boo, V803 Cen and CP Eri are VY Scl analogues, with unstable mass transfer caused by irradiative effects. GP Com is the equivalent of an SU UMa star at quiescent, and would be expected to show superoutbursts on intervals of decades. The AM CVn stars should be the strongest gravitational radiation emission line sources in the 0.7-2.0 mHz range.
引用
收藏
页码:249 / 270
页数:22
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