The structure of the common envelope in a close binary system

Details The structure of the common envelope in a close binary system The structure of the common envelope in a close binary system

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009arep...53..223s&link_type=abstract

Astronomy Reports, Volume 53, Issue 3, pp.223-231

Astronomy and Astrophysics

Astronomy

5

97.80.Fk, 97.10.Fy, 97.10.Gz, Spectroscopic Binaries, Close Binaries, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Accretion And Accretion Disks

Scientific paper

As a result of the interaction between an elliptical accretion disk and gas flowing into it from the circumbinary envelope in a close binary in the course of its orbital motion, the matter of the disk and the circum-disk halo is periodically ejected from the vicinity of the Lagrange point L3, and a common envelope is formed in the system. Three-dimensional numerical gas-dynamical modeling is used to study the structure and dynamics of the envelope and determine its basic parameters. The evolution of the envelope is followed on timescales of the order of several orbital periods. The matter flow ejected through the vicinity of L3 displays a spiral shape. The maximum size of the forming spiral structure is restricted by the self-intersection point, and is of the order of four to five times the component separation. We consider the dynamics of the regions directly adjacent to the spiral structure: an inner, rarified and outer, fragmented region, which further makes a transition to an expanding diffuse ring.

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