Investigations of the Accretion Disc Structure in SS Cyg Using the Doppler Tomography Technique

Details Investigations of the Accretion Disc Structure in SS Cyg Using the Doppler Tomography Technique Investigations of the Accretion Disc Structure in SS Cyg Using the Doppler Tomography Technique

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1121...17k&link_type=abstract

SPACE PLASMA PHYSICS: School of Space Plasma Physics. AIP Conference Proceedings, Volume 1121, pp. 17-21 (2009).

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Novae, Dwarf Novae, Recurrent Novae, And Other Cataclysmic Variables, Astronomical And Space-Research Instrumentation, Planetary Bow Shocks, Interplanetary Shocks, Infall, Accretion, And Accretion Disks, X-Ray Binaries

Scientific paper

Using spectra obtained on the 2-meter telescope Zeiss-2000 (Terskol, Russia) during quiescent and active states of the system along with results of 3D gas dynamical simulations we investigated the structure of the matter flow and parameters of the accretion disk in the system in quiescent and active states. We show that during quiescence in the system following gas dynamic elements exist: accretion disk, arms of the spiral tidal shock, shock front due to the interaction between the gas of the circum-binary envelope and the stream from the inner Lagrangian point (the ``hot line''), and in the region behind the bow shock forming due to the motion of the accretor and disk in the gas of the envelope. The contribution of this last element results in appreciable asymmetry of the tomograms. The phenomenological model of an SS Cyg outburst is proposed. According to the model the structure of the gas dynamic pattern changes during an outburst and it consists of the accretion disk, a toroidal shell formed in the inner parts of the disk, an expanding spherical shell around the accreting star, a region in front of the bow shock, and the surface of the donor star near the inner Lagrangian point, L1, which is heated by radiation from the accretor.

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