Doppler mapping of the SS Cyg system during outburst

Boneva, Daniela; Kaigorodov, P. V.; Bisikalo, D. V.; Kononov, D. A.

doi:10.1134/s1063772909110055

Cited by 9 publications

(8 citation statements)

References 2 publications

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“…This method transforms the orbital variability of emission-line intensities into luminosity maps in the two-dimensional velocity space (V x , V y ). In the papers of Bisikalo et al (2008); Kononov et al (2008); and Boneva et al (2009), SS Cygni was investigated using Doppler tomography in addition to three-dimensional (3D) gas dynamic simulations. This approach allowed the authors to identify the main gas dynamical elements existing in the system in the quiescent state (immediately after an outburst) and at a late stage of the outburst.…”

Section: Introductionmentioning

confidence: 99%

Structure of the pre-outburst accretion disk in SS Cygni

Kononov

Giovannelli

Bruni

et al. 2012

A&A

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We present results of spectroscopic observations of SS Cygni performed at the 1.5 m telescope of the Loiano Observatory in June 2009, three days before a long outburst. Using results of these observations, we computed Doppler tomograms in three Balmer lines H β , H γ , and H δ . Analyzing the tomograms, we identified gas dynamic features existing in the system. It is shown that in the preoutburst disk a number of shock waves exist. These waves are "hot line" a wave produced by the interaction between the circum-disk halo and the stream from the inner Lagrangian point L 1 , and two arms of the spiral tidal shock and bow shock caused by the motion of the accretor and disk in the gas of the circum-binary envelope. We also found that before the outburst the density and size of the disk increase.

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Section: Introductionmentioning

confidence: 99%

Structure of the pre-outburst accretion disk in SS Cygni

Kononov

Giovannelli

Bruni

et al. 2012

A&A

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“…We have derived Hβ and Hγ Doppler tomograms for SS Cyg in its active state from spectral observations of the star, see papers [17], [18].…”

Section: Resultsmentioning

confidence: 99%

Models of Vortices and Spirals in White Dwarf’s Accretion Binaries

Boneva¹

2010

AIP Conference Proceedings

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Abstract.The main aim in the current survey is to suggest models of the development of structures, such as vortices and spirals, in accretion white dwarf's binaries. Numerical methods and simulations are applied on the bases of hydrodynamic analytical considerations. It is suggested in the theoretical model the perturbation's parameters of the accretion flow, which are caused by the influences of the tidal wave over the flux of accretion matter around the secondary star. The results of numerical code application on the disturbed flow reveal an appearing of structure with spiral shape due to the tidal interaction in the close binaries. Our further simulations give the solution, which expresses the formation of vortical configurations in the accretion disc's zone. The evolution of vortices in areas of the flow's interaction is explored using single vortex and composite vortex models. Gas in the disc matter is considered to be compressible and non-ideal. The longevity of all these structures is different and each depends on the time period of the rotation, density and velocity of the accretion matter.

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“…Thus, apart from night 2, the outburst data are not consistent with the orbital period, with two shorter periods and one longer one. There is a temptation to consider the night 3 data as evidence for a positive superhump - Boneva et al (2009) suggested that in outburst SS Cyg has an elliptical disc. If so, SS Cyg is not impossibly far off the standard P sh , P orb relation, and the orbital period of 6.6 h would be the longest on that relation.…”

Section: Photometrymentioning

confidence: 99%

SS Cygni Revisited

Smith

Echevarría²,

Szkody

2015

APP

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New spectroscopic and photometric observations of SS Cygni, the brightest dwarf nova system, have been obtained, with the aim of mapping starspots on the surface of the secondary star. Four nights of echelle spectroscopy in quiescence have been obtained using the 2.2-m telescope at San Pedro Martir (Mexico) in August 2012 and another two nights at the 3.5-m telescope at Apache Point Observatory, USA, in September 2012, but these data are still being reduced. Simultaneous CCD photometry was also obtained at the two sites, and the Mexican photometry was extended into the subsequent long outburst. This presentation reveals some interesting photometric behaviour in that outburst, but further data will be necessary before the nature of the behaviour can be determined.

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Doppler mapping of the SS Cyg system during outburst

Cited by 9 publications

References 2 publications

Structure of the pre-outburst accretion disk in SS Cygni

Structure of the pre-outburst accretion disk in SS Cygni

Models of Vortices and Spirals in White Dwarf’s Accretion Binaries

SS Cygni Revisited

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