The matter-flow structure in the SS Cyg system in its quiescent state from comparisons of observational and synthetic Doppler tomograms

Бисикало, Д. В.; Kononov, D. A.; Kaigorodov, P. V.; Жилкин, А. Г.; Boyarchuk, A. A.

doi:10.1134/s1063772908040069

Cited by 22 publications

(27 citation statements)

References 10 publications

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“…To explain the observed details of the tomograms, we consider the results of gas dynamic simulations performed following the approach of Bisikalo et al (2008). In Fig.…”

Section: Resultsmentioning

confidence: 99%

“…If we assume that the bright spots in the tomograms are shock waves (e.g. Bisikalo et al 2008), one can see that in the H δ tomogram the shock waves have the highest intensity relative to the background. Thus, probably, in H δ we see mostly the radiation of the shock waves.…”

Section: Doppler Tomogramsmentioning

confidence: 99%

“…1, were obtained using the 2-m telescope of the observatory located at Terskol peak (Caucasus, Russia). Observations and data reduction were described in Bisikalo et al (2008). To preserve the uniformity of the data in both the sets, we used the same reduction procedure for both of them.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Using them, we aim to investigate the structure of the pre-outburst disk in SS Cygni. In addition, we use spectroscopic data, tomograms, and the results of the gas dynamic simulations of Bisikalo et al (2008). They were acquired at the beginning of the quiescent state immediately after a short outburst.…”

Section: Introductionmentioning

confidence: 99%

“…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%

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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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“…To explain the observed details of the tomograms, we consider the results of gas dynamic simulations performed following the approach of Bisikalo et al (2008). In Fig.…”

Section: Resultsmentioning

confidence: 99%

Section: Doppler Tomogramsmentioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Structure of the pre-outburst accretion disk in SS Cygni

Kononov

Giovannelli

Bruni

et al. 2012

A&A

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The effect of diffusion of magnetic field on flow structure in close binaries

Жилкин

Bisikalo

2010

Advances in Space Research

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Voracious vortices in cataclysmic variables

Neustroev

Zharikov²

2020

A&A

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Context. In Paper I we showed that the accretion disc radius of the dwarf nova HT Cas in its quiescent state has not changed significantly during many years of observations. It has remained consistently large, close to the tidal truncation radius. This result is inconsistent with the modern understanding of the evolution of the disc radius through an outburst cycle. Aims. Spectroscopic observations of HT Cas during its superoutburst offered us an exceptional opportunity to compare the properties of the disc of this object in superoutburst and in quiescence. Methods. We obtained a new set of time-resolved spectra of HT Cas in the middle of its 2017 superoutburst. We used Doppler tomography to map emission structures in the system, which we compared with those detected during the quiescent state. We used solutions of the restricted three-body problem to discuss again the location of emission structures and the disc size of HT Cas in quiescence. Results. The superoutburst spectrum is similar in appearance to the quiescent spectra, although the strength of most of the emission lines decreased. However, the high-excitation lines significantly strengthened in comparison with the Balmer lines. Many lines show a mix of broad emission and narrow absorption components. Hα in superoutburst was much narrower than in quiescence. Other emission lines have also narrowed in outburst, but they did not become as narrow as Hα. Doppler maps of Hα in quiescence and of the Hβ and He I lines in outburst are dominated by a bright emission arc at the right side of the tomograms, which is located at and even beyond the theoretical truncation limit. However, the bulk of the Hα emission in outburst has significantly lower velocities. Conclusions. We show that the accretion disc radius of HT Cas during its superoutburst has become hot but remained the same size as it was in quiescence. Instead, we detected cool gas beyond the Roche lobe of the white dwarf that may have been expelled from the hot disc during the superoutburst.

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The matter-flow structure in the SS Cyg system in its quiescent state from comparisons of observational and synthetic Doppler tomograms

Cited by 22 publications

References 10 publications

Structure of the pre-outburst accretion disk in SS Cygni

Structure of the pre-outburst accretion disk in SS Cygni

The effect of diffusion of magnetic field on flow structure in close binaries

Voracious vortices in cataclysmic variables

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