Accretion disk limit cycle mechanism in twin-degenerate interacting binaries

Details Accretion disk limit cycle mechanism in twin-degenerate interacting binaries Accretion disk limit cycle mechanism in twin-degenerate interacting binaries

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.311..443c&link_type=abstract

Nature (ISSN 0028-0836), vol. 311, Oct. 4, 1984, p. 443, 444.

Statistics

Computation

21

Accretion Disks, Binary Stars, Dwarf Novae, Light Curve, Stellar Flares, Stellar Mass Accretion, Computational Astrophysics, Stellar Models, Variable Stars, White Dwarf Stars

Scientific paper

The twin-degenerate interacting binary stars are thought to consist of two pure helium white dwarfs in close orbit. The candidates are G61-29 (also GP Com), HZ 29 (also AM CVn) and, tentatively, PG1346+082. Large variations in the optical light of PG1346+082 suggest variable accretion onto the star gaining mass. Such behaviour is thought to be caused by either episodic mass overflow from the mass-losing star or the instability in the accretion disk. The authors investigate the latter mechanism, and explore the non-thermal equilibrium limit cycle behaviour of the accretion disk expected for a twin-degenerate interacting binary system.

Affiliated with

Also associated with

No associations

Rating

Accretion disk limit cycle mechanism in twin-degenerate interacting binaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Accretion disk limit cycle mechanism in twin-degenerate interacting binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Accretion disk limit cycle mechanism in twin-degenerate interacting binaries will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1229405