The formation and evolution of accretion disks in binary systems

Details The formation and evolution of accretion disks in binary systems The formation and evolution of accretion disks in binary systems

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ap%26ss.182...61h&link_type=abstract

Astrophysics and Space Science, Volume 182, Issue 1, pp.61-68

Astronomy and Astrophysics

Astrophysics

Scientific paper

In this paper, we consider a close binary system consisting of a compact star and a optical Main-Sequence star which fills its critical Roche lobe and transfers matter through the inner Lagrangian pointL 1 toward the compact object. We use the Hill's problem as the dynamical model of the binaries. The following binaries are calculated by Duncanet al.'s mapping approximation: RY Per, RZ Sct, RS Vul, and λ Tau. Figures 3 6 show that the trajectories of accretion disk particles in the binaries. The relation between the dimensionless semi-major axis ɛ and times of conjunctionN are presented in Figures 7 10.

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