Inner Edge Drag by the Compact Star and Disc Structure and Dynamics in Close Binary Systems: 3D SPH Numerical Experiments

Details Inner Edge Drag by the Compact Star and Disc Structure and Dynamics in Close Binary Systems: 3D SPH Numerical Experiments Inner Edge Drag by the Compact Star and Disc Structure and Dynamics in Close Binary Systems: 3D SPH Numerical Experiments

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasj...49..329b&link_type=abstract

Publications of the Astronomical Society of Japan, v.49, p.329-340.

Astronomy and Astrophysics

Astronomy

Accretion, Accretion Discs, Hydrodynamics, Numerical Methods, Stars: Binaries, Stars: Mass Loss, Stars: Rotation, Stars: White Dwarfs

Scientific paper

The aim of this work is to study the effect of the drag exerted by an asynchronous primary on accretion disc structure and dynamics in an interacting close binary system. Comparison of two 3D SPH disc simulations has been performed, the first relative to the customary synchronous case, the second to an asynchronous one, assuming the primary rotational axis to be perpendicular to the orbital plane, and, in the latter case, the rotational angular velocity to be twice the orbital one, namely omega = 2 omega_ °. Some tests have been carried out also in the cases: omega = 1.5 omega_ °, omega = 5 omega_ ° and omega = 10 omega_ °, where omega is the primary angular velocity and omega_ ° is the orbital angular velocity. The results relative to the omega = 2 omega_ ° model show a hot accretion disc whose inner edge is characterized by an asymmetric rotational motion, an azimuthal compression wave and a rotating local bump, which may explain luminosity variations observed in close binary systems. A hot wind coming from the outer edge of the disc is also found. In this asynchronous model the accretion and ejection mass rates are lower and higher respectively, in comparison to those characteristic of the synchronous model. For faster rotation rates omega , the tests performed indicate that high ejection mass rates, both from the outer and inner edges, do not allow the development of a well defined accretion disc.

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