V2051 Oph's disc evolution on decline from superoutburst

@article{Vrielmann2002V2051OD,
  title={V2051 Oph's disc evolution on decline from superoutburst},
  author={Sonja Vrielmann and Warren B. Offutt},
  journal={arXiv: Astrophysics},
  year={2002}
}
We present an Eclipse Mapping analysis of ten eclipses taken during decline from superoutburst of the dwarf nova V2051 Oph. On decline from superoutburst the disc cools down considerably from nearly 50,000 K in the intermediate disc (approx. 0.2 R_L1) near maximum to about 25,000 K at the end of our observing run, i.e. within 4 days. The average mass accretion rate through the disc drops in the same time from 10^18 g/s to below 10^17 g/s. While in some maps the brightness temperature follows… Expand
7 Citations

Figures and Tables from this paper

A Study of the Evolution of the Accretion Disk of V2051 Ophiuchi through Two Outburst Cycles
We follow the changes in the structure of the accretion disk of the dwarf nova V2051 Oph along two separate outbursts in order to investigate the causes of its recurrent outbursts. We applyExpand
Infrared photometry of the dwarf nova V2051 Ophiuchi – II. The quiescent accretion disc and its spiral arms
We report the analysis of time-series of infrared $JHK_s$ photometry of the dwarf nova V2051 Oph in quiescence with eclipse mapping techniques to investigate structures and the spectrum of itsExpand
Infrared photometry of the dwarf nova V2051 Ophiuchi - I. The mass-donor star and the distance
We report the analysis of time-series of infrared $JHK_s$ photometry of the dwarf nova V2051 Oph in quiescence. We modelled the ellipsoidal variations caused by the distorted mass-donor star to inferExpand
Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VIII: The Eighth Year (2015-2016)
Continuing the project described by Kato et al. (2009, arXiv:0905.1757), we collected times of superhump maxima for 128 SU UMa-type dwarf novae observed mainly during the 2015-2016 season andExpand
Global MHD Simulations of Accretion Disks in Cataclysmic Variables (CVs): II The Relative Importance of MRI and Spiral Shocks
We perform global three-dimensional MHD simulations of unstratified accretion disks in cataclysmic variables (CVs). By including mass inflow via an accretion stream, we are able to evolve the disk toExpand
Period changes of cataclysmic variables below the period gap: V2051 Oph, OY Car and Z Cha
Abstract We present our results of a long-term monitoring of cataclysmic variable stars (CVs). About 40 new eclipses were measured for the three southern SU UMa-type eclipsing CVs: V2051 Oph, OY CarExpand
Long-term Periodicities of Cataclysmic Variables with Synoptic Surveys
A systematic study on the long-term periodicities of known Galactic cataclysmic variables (CVs) was conducted. Among 1580 known CVs, 344 sources were matched and extracted from the Palomar TransientExpand

References

SHOWING 1-6 OF 6 REFERENCES
Cataclysmic Variable Stars - How and Why They Vary
Introduction.- Orbital Lightcurves and Eclipses.- The Dwarf Nova Eruption.- Tidal Instabilities in Accretion Discs.- Magnetic Systems.- Low States and Secondary Star Variability.- Flickering,Expand
The Cataclysmic Variable Stars
Preface 1. Historical development 2. Structure of non-magnetic systems 3. Dwarf novae 4. Nova-like variables and nova remnants 5. Novae in eruption 6. Polars 7. Intermediate polars 8. DQ HerculisExpand
Cataclysmic Variables: a 60th Birthday Symposium in Honour of Brian Warner
  • Cataclysmic Variables: a 60th Birthday Symposium in Honour of Brian Warner
  • 1997
Accretion Discs in compact systems
  • Accretion Discs in compact systems
  • 1993
Advanced Series in Astrophysics and Cosmology
  • Advanced Series in Astrophysics and Cosmology
  • 1993
Cataclysmic Variables: a 60th Birthday Symposium in Honour of Brian Warner
  • Warner Symposium Proceedings