# The dwarf nova SS Cygni: what is wrong?

@article{Schreiber2007TheDN,
title={The dwarf nova SS Cygni: what is wrong?},
author={Matthias R. Schreiber and Jan Lasota},
journal={arXiv: Astrophysics},
year={2007}
}
• Published 26 June 2007
• Physics
• arXiv: Astrophysics
Since the Fine Guiding Sensor (FGS) on the Hubble Space Telescope (HST) was used to measure the distance to SS Cyg to be $166\pm12$ pc, it became apparent that at this distance the disc instability model fails to explain the absolute magnitude during outburst. It remained, however, an open question whether the model or the distance have to be revised. Recent observations led to a revision of the system parameters of SS Cyg and seem to be consistent with a distance of $d\gta 140$ pc. We re…
28 Citations

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## References

SHOWING 1-10 OF 29 REFERENCES
Delays in dwarf novae I: The case of SS Cygni
• Physics
• 2003
Using the disc instability model and a simple but physically reasonable model for the X-ray, extreme UV, UV and optical emission of dwarf novae we investigate the time lags observed between the rise
Implications of the HST/FGS parallax of SS Cygni on the disc instability model
• Physics
• 2002
We analyse the consequences of the recently measured parallax of SS Cygni (Harrison et al. 1999) on the accretion disc limit cycle model. Using the observed long term light curve of SS Cyg and d =
The Masses and Evolutionary State of the Stars in the Dwarf Nova SS Cygni
• Physics, Geology
• 2007
The dwarf nova SS Cygni is a close binary star consisting of a K star transferring mass to a white dwarf by way of an accretion disk. We have obtained new spectroscopic observations of SS Cyg. Fits
Z Cam stars: A particular response to a general phenomenon
• Physics
• 2001
We show that the disc instability model can reproduce all the observed properties of Z Cam stars if the energy equation includes heating of the outer disc by the mass-transfer stream impact and by
WX Ceti : a closer look at its behaviour in quiescence and outburst
• Physics
• 2007
Context. WX Cet is a dwarf nova with rare outbursts of large amplitude. Aims. We compile the available data of WX Cet, compare the results with other SU UMa stars, and discuss our findings in the
AN ASTROMETRIC CALIBRATION OF THE MV-PORB RELATIONSHIP FOR CATACLYSMIC VARIABLES BASED ON HUBBLE SPACE TELESCOPE FINE GUIDANCE SENSOR PARALLAXES
• Physics
• 2004
We present new, high-precision astrometric parallaxes for three cataclysmic variables: WZ Saggitae, YZ Cancri, and RU Pegasi, obtained using the Fine Guidance Sensors on the Hubble Space Telescope.
Delays in dwarf novae II: VW Hyi, the tidal instability and enhanced mass transfer models
• Physics
• 2004
We discuss the multi-wavelength predictions of the two models proposed for SU UMa stars, i.e. the enhanced mass transfer (EMT) and the tidal thermal instability (TTI) models. We focus on the
The masses, radii and luminosities of the components of U Geminorum
• Physics, Geology
• 2005
We present a phase-resolved spectroscopic study of the secondary star in the cataclysmic variable (CV) U Gem. We use our data to measure the radial velocity semi-amplitude, systemic velocity and
A spectroscopic search for faint secondaries in cataclysmic variables
• Physics
• 2003
The secondary in cataclysmic variables (CVs) is usually detected by cross-correlation of the CV spectrum with that of a K or M dwarf template, to produce a radial velocity curve. Although this method