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}
}
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… 

Figures and Tables from this paper

On the Hubble Space Telescope Trigonometric Parallax of the Dwarf Nova SS Cygni
SS Cygni is one of the brightest dwarf novae (DNe), and one of the best-studied prototypes of the cataclysmic variables. Astrometric observations with the Fine Guidance Sensors (FGS) on the Hubble
An Accurate Geometric Distance to the Compact Binary SS Cygni Vindicates Accretion Disc Theory
TLDR
Using very long baseline interferometric radio observations, an accurate, model-independent distance is derived to SS Cygni that places the source substantially closer, reconciling the source behavior with the understanding of accretion disc theory in accreting compact objects.
Anomalous Z Cam stars: a response to mass-transfer outbursts
Recent observations of two unusual Z Cam systems, V513 Cas and IW And have shown light curves that seem to contradict the disc-instability model for dwarf novae: outbursts are appearing during
Dwarf nova outbursts in intermediate polars
The disc instability model (DIM) has been very successful in explaining the dwarf nova outbursts observed in cataclysmic variables. When, as in intermediate polars (IP), the accreting white dwarf is
Testing the disk instability model of cataclysmic variables
Context. The disk instability model (DIM) attributes the outbursts of dwarf novae to a thermal-viscous instability of their accretion disk, an instability to which nova-like stars are not subject.
Distances of cataclysmic variables and related objects derived from Gaia Data Release 1
We consider the parallaxes of sixteen cataclysmic variables and related objects that are included in the TGAS catalogue, which is part of the Gaia first data release, and compared these with previous
The reproducible radio outbursts of SS Cygni
We present the results of our intensive radio observing campaign of the dwarf nova SS Cyg during its 2010 April outburst. We argue that the observed radio emission was produced by synchrotron
THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS
We present an attempt to reconstruct the complete evolutionary path followed by cataclysmic variables (CVs), based on the observed mass-radius relationship of their donor stars. Along the way, we
One Good Measure
TLDR
Radio observations show that the HST distance measure is wrong and that instead SS Cygni is exactly as far away as it should be according to the understanding of accretion disks.
The decline in irradiation from the white dwarf in old novae
Aims. We have investigated how a flux ratio analysis of the light curves of cataclysmic variables can be used to calculate the luminosity irradiating the secondary star in the classical novae QU Vul,
...
...

References

SHOWING 1-10 OF 29 REFERENCES
Delays in dwarf novae I: The case of SS Cygni
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
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
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
Unsolved problems of dwarf nova outbursts
Z Cam stars: A particular response to a general phenomenon
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
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
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
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
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
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
...
...