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On the Mass Transfer Rate in SS Cyg

Smak J.

Acta Astronomica

2010

Vol. 60, No. 1

83--89

The mass transfer rate in SS Cyg at quiescence, estimated from the observed luminosity of the hot spot, is log Mtr=16.8±0.3. This is safely below the critical mass transfer rates of log Mcrit=18.1 (corresponding to log Tcrit0=3.88) or log Mcrit=17.2 (corresponding to the "revised" value of log Tcrit0=3.65). The mass transfer rate during outbursts is strongly enhanced.

On the Interpretation of Doppler Tomograms of Dwarf Nova Disks During Outbursts

Smak J.

Acta Astronomica

2001

Vol. 51, No. 3

295--302

Simple model of the disk based on purely mechanical, restricted three-body approximation is already sufficient to explain the presence and shapes of the two arch-like structures observed in Doppler tomograms of dwarf nova disks during their outbursts. In particular, it explains their non-equal intensities (which could not be explained by the 2D hydrodynamic, spiral-wave models).

Hα Observations of SS Cyg at Quiescence and Outburst

Marchev D., Kjurkchieva D., Ogłoza W.

Acta Astronomica

1999

Vol. 49, No. 4

585--598

Observations of Hα line of SS Cyg at quiescence and outburst are presented. The corresponding radial velocity curve is sinusoidal with semiamplitude K1=91±3.5 km/s. The width and intensity of the Hα line during quiescence are slightly variable. Its profile shape changes quite irregular but does not show the typical double-peaked structure of an accretion disk. The small peaks at the profile cores form S-wave with half-orbital period. The Hα profiles of SS Cyg at outburst consist of central emission core superposed on wide shallow absorption base. The intensity of the emission core is almost the same as that of the emission line in quiescence. The double-peaked shape of the profile is not well pronounced during the outburst too. On the base of the parameters of the Hα profile we estimate that the condition for the existence of an accretion disk during quiescence is not fulfilled. Such a structure can exist in outburst but it cannot be a dominant source of the Hα emission. Taking into account similarity of SS Cyg and the polar AM Her we conclude that the Balmer emission of SS Cyg originates mostly from the polar caps.