Dynamical instability model for the period gap of cataclysmic variable binary sytems
A dynamical instability in a convective secondary is proposed as an explanation of the period gap of cataclysmic variable systems. It is demonstrated that if, during the course of evolution of the binary system, the secondary component detaches from its Roche lobe when it is fully convective, then at the next onset of mass transfer a dynamical instability may ensue. It is shown that such a system at orbital period near 3 hr will be unstable to mass transfer and that stability will be regained at longer orbital periods when the system becomes detached. If the time scale for orbital decay by angular momentum losses associated with gravitational radiation and/or a magnetically coupled stellar wind is shorter than the Hubble time, the system will then resume mass transfer at periods near 2 hr. 23 references.
- Research Organization:
- Northwestern Univ., Evanston, IL
- OSTI ID:
- 5839212
- Journal Information:
- Astrophys. J.; (United States), Vol. 319
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
GENERAL PHYSICS
ERUPTIVE VARIABLE STARS
STAR MODELS
ANGULAR MOMENTUM
BINARY STARS
GRAVITATIONAL WAVES
LUMINOSITY
MASS
MASS TRANSFER
STABILITY
STAR EVOLUTION
STELLAR WINDS
WHITE DWARF STARS
DWARF STARS
MATHEMATICAL MODELS
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
STARS
STELLAR ACTIVITY
VARIABLE STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
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