Structure of the pre-outburst accretion disk in SS Cygni

Kononov, D. A.; Giovannelli, F.; Bruni, I.; Bisikalo, D. V.

doi:10.1051/0004-6361/201016334

Cited by 15 publications

(13 citation statements)

References 19 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Indeed, our observations are consistent with those by Kononov et al (2012), who found a similar asymmetric emission in the right-hand quadrants. We also find increased emission in the lower-left quadrant of the Hγ map, similar to that found in the Hα tomogram of North et al (2002), as well as the Hγ and Hδ tomograms of Kononov et al (2012). However, there are also differences between our tomograms and those of Kononov et al (2012), confirming their conclusions of changes in the accretion disk between outbursts.…”

Section: Emission Line Featuressupporting

confidence: 94%

Roche tomography of cataclysmic variables – VIII. The irradiated and spotted dwarf nova, SS Cygni

Hill

Smith

Hebb

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the results of our spectroscopic study of the dwarf nova SS Cyg, using Roche tomography to map the stellar surface and derive the system parameters. Given that this technique takes into account the inhomogeneous brightness distribution on the surface of the secondary star, our derived parameters are (in principle) the most robust yet found for this system. Furthermore, our surface maps reveal that the secondary star is highly spotted, with strongly asymmetric irradiation on the inner hemisphere. Moreover, by constructing Doppler tomograms of several Balmer emission lines, we find strong asymmetric emission from the irradiated secondary star, and an asymmetric accretion disc that exhibits spiral structures.

show abstract

Section: Emission Line Featuressupporting

confidence: 94%

Roche tomography of cataclysmic variables – VIII. The irradiated and spotted dwarf nova, SS Cygni

Hill

Smith

Hebb

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…IP Peg (eg. Steeghs & Stehle 1999;Morales-Rueda et al 2000), SS Cyg (Steeghs et al 1996;Kononov et al 2012), EX Dra (Joergens et al 2000a,b), U Gem (eg. Groot 2001) and WZ Sge (Baba et al 2002;Steeghs 2004).…”

Section: Discussionmentioning

confidence: 99%

A spectroscopic analysis of the eclipsing nova-like EC 21178−5417 – discovery of spiral density structures

Khangale

Woudt

Potter

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present phase-resolved optical spectroscopy of the eclipsing nova-like cataclysmic variable EC21178-5417 obtained between 2002 and 2013. The average spectrum of EC21178-5417 shows broad double-peaked emission lines from HeII 4686Å (strongest feature) and the Balmer series. The high-excitation feature, CIII/NIII at 4640-4650Å, is also present and appears broad in emission. A number of other lines, mostly HeI, are clearly present in absorption and/or emission. The average spectrum of EC21178-5417 taken at different months and years shows variability in spectral features, especially in the Balmer lines beyond Hγ, from pure line emission, mixed line absorption and emission to pure absorption lines. Doppler maps of the HeII 4686Å emission reveal the presence of a highly-inclined asymmetric accretion disc and a two spiral armlike structure, whereas that of the Balmer lines (Hα and Hβ) reveal a more circular accretion disc. There is no evidence of a bright spot in the Doppler maps of EC21178-5417 and no emission from the secondary star is seen in the tomograms of the HeII 4686Å and Balmer lines. Generally, the emission in EC21178-5417 is dominated by emission from the accretion disc. We conclude that EC21178-5417 is a member of the RW Tri or UX UMa sub-type of nova-like variables based on these results and because it shows different spectral characteristics at different dates. This spectral behaviour suggests that EC21178-5417 undergoes distinct variations in mass transfer rate on the observed time scales of months and years.

show abstract

“…However, Bisikalo et al (1998) pointed out that in high-mass-transfer rate binaries, the matter can escape the accretion disc and create a halo around the disc. According to their three-dimensional gas-dynamical simulations of accretion flows in a 5.4-h system with typical stellar parameters and a mass-transfer rate of 10 −8 M ⊙ /year, an extended low-velocity region (hereafter called an 'outflow zone') is filled with matter pouring from the disc (Bisikalo et al 2008;Kononov et al 2012). This region is located practically on the opposite side of the disc with respect to the hotspot (labelled as A and B in fig.…”

Section: Accretion Flow Structure In Long-period Nl Systemsmentioning

confidence: 99%

Structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451

Hernández

Zharikov

Neustroev

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

New time-resolved optical spectroscopic echelle observations of the nova-like cataclysmic variable RW Sextantis were obtained, with the aim to study the properties of emission features in the system. The profile of the Hα emission line can be clearly divided into two ('narrow' and 'wide') components. Similar emission profiles are observed in another nova-like system, 1RXS J064434.5+33445, for which we also reanalysed the spectral data and redetermined the system parameters. The source of the 'narrow', low-velocity component is the irradiated face of the secondary star. We disentangled and removed the 'narrow' component from the Hα profile to study the origin and structure of the region emitting the wide component. We found that the 'wide' component is not related to the white dwarf or the wind from the central part of the accretion disc, but is emanated from the outer side of the disc. Inspection of literature on similar systems indicates that this feature is common for some other long-period nova-like variables. We propose that the source of the 'wide' component is an extended, low-velocity region in the outskirts of the opposite side of the accretion disc, with respect to the collision point of the accretion stream and the disc.

show abstract

Structure of the pre-outburst accretion disk in SS Cygni

Cited by 15 publications

References 19 publications

Roche tomography of cataclysmic variables – VIII. The irradiated and spotted dwarf nova, SS Cygni

Roche tomography of cataclysmic variables – VIII. The irradiated and spotted dwarf nova, SS Cygni

A spectroscopic analysis of the eclipsing nova-like EC 21178−5417 – discovery of spiral density structures

Structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451

Contact Info

Product

Resources

About