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Outburst Cycle of the Dwarf Nova SS Cygni

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Abstract

Extensive observational data obtained to date is analyzed with special attention given to space observations. The spectral type of the white dwarf is estimated and it is concluded that accretion of matter on it is the only source of the x-ray flux in the system. The rotation of the secondary is shown to be synchronous and therefore its illumination by hard x-rays results in the formation of stellar wind. This is the main mechanism of mass transfer onto the white dwarf. The geometry of the system prevents the formation of the disk by stellar wind. Instead, stellar wind forms a quasispherical envelope whose variability influences the outburst process. Based on these conclusions, the properties of the system are interpreted, which so far have remained unexplained: short-term appearance of peculiar spectrum during the rising phase of the outburst, rather constant width of absorption lines during the outburst, decrease of the width of emission lines during the outburst, variation of the x-ray and ultraviolet fluxes during ordinary and low-amplitude anomalous outbursts, and, finally, the quasiperiodicity of the outbursts.

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Authors and Affiliations

  1. Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, 369167, Russia

    N. F. Voikhanskaya

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  1. N. F. Voikhanskaya
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Correspondence to N. F. Voikhanskaya.

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Original Russian Text © N.F. Voikhanskaya, 2018, published in Astrofizicheskii Byulleten’, 2018, Vol. 73, No. 1, pp. 88–101.

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Voikhanskaya, N.F. Outburst Cycle of the Dwarf Nova SS Cygni. Astrophys. Bull. 73, 84–97 (2018). https://doi.org/10.1134/S1990341318010078

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  • DOI: https://doi.org/10.1134/S1990341318010078

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