Accretion Disk Model of Dwarf Novae

Details Accretion Disk Model of Dwarf Novae Accretion Disk Model of Dwarf Novae

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982pthph..67..179h&link_type=abstract

Progress of Theoretical Physics, Vol. 67, No. 1, pp. 179-189

Physics

3

Scientific paper

We develop a theory of accretion disks surrounding white dwarfs on the basis of the α-model of viscous stress. We wish to point out that when the accretion rate is less than ˜1015gm\cdots-1, two physically distinct states exist depending on the temperature of the accreting material; the accretion gas develops into an optically thin and high temperature disk or forms a low temperature ring. It is also found that in the rise phase of an outburst the appearance of the soft X-rays delays for about one day relative to the optical outburst. We apply these results to construct a model of SS Cygni and U Geminorum.

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