Doppler tomography of the dwarf novae VY Aquari and WX Ceti

Mennickent, R. E.; Unda-Sanzana, E.; Tappert, C.

doi:10.1051/0004-6361:20064850

Cited by 4 publications

(3 citation statements)

References 26 publications

(32 reference statements)

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“…Most studies are confined to using the strong Balmer emission lines to try and constrain system parameters (e.g. table 2 in Szkody, Desai & Hoard 2000; Marsh 2001; Mennickent, Unda‐Sanzana & Tappert 2006; Southworth et al 2007; Neilsen, Steeghs & Vrtilek 2008).…”

Section: Gw Lib Post Outburstmentioning

confidence: 99%

Time-resolved spectroscopy of the pulsating CV GW Lib

Spaandonk

Steeghs

Marsh

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present time-resolved optical spectroscopy of the dwarf nova GW Librae during its rare April 2007 super-outburst and compare these with quiescent epochs. The data provide the first opportunity to track the evolution of the principal spectral features. In the early stages of the outburst, the optically thick disc dominates the optical and the line components show clear orbital radial velocity excursions. In the course of several weeks, optically thin regions become more prominent as strong emission lines replace the broad disc absorption. Post-outburst spectroscopy covering the I-band illustrates the advantages of CaII relative to the commonly used Balmer lines when attempting to constrain binary parameters. Due to the lower ionisation energy combined with smaller thermal and shear broadening of these lines, a sharp emission component is seen to be moving in between the accretion disc peaks in the CaII line. No such component is visible in the Balmer lines. We interpret this as an emission component originating on the hitherto unseen mass donor star. While our conservative dynamical limits place a hard upper limit on the binary mass ratio of q<0.23, we favour a significantly lower value near q~0.06. Pulsation modeling suggests a WD mass ~1 M_sun. This, paired with a low mass donor, near the empirical sequence of an evolved CV close to the period bounce, appears to be consistent with all the observational constraints to date. [abridged]Comment: Accepted for publication in MNRAS. 13 pages with 5 tables and 7 figure

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Section: Gw Lib Post Outburstmentioning

confidence: 99%

Time-resolved spectroscopy of the pulsating CV GW Lib

Spaandonk

Steeghs

Marsh

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…11 See, for examples, the Doppler maps of SU UMa-type systems inRodríguez-Gil et al (2005),Mennickent et al (2006), Longa-Peña et al (2015,Littlefield et al (2018).…”

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confidence: 99%

The period-gap cataclysmic variable CzeV404 Her: A link between SW Sex and SU UMa systems

Kára

Zharikov

Wolf

et al. 2021

A&A

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Context. We present a new study of the eclipsing cataclysmic variable CzeV404 Her (Porb = 0.098 d) that is located in the period gap. Aims. This report determines the origin of the object and the system parameters and probes the accretion flow structure of the system. Methods. We conducted simultaneous time-resolved photometric and spectroscopic observations of CzeV404 Her. We applied our light-curve modelling techniques and the Doppler tomography method to determine the system parameters and analyse the structure of the accretion disk. Results. We found that the system has a massive white dwarf MWD = 1.00(2) M⊙, a mass ratio of q = 0.16, and a relatively hot secondary with an effective temperature T2 = 4100(50) K. The system inclination is i = 78.8°. The accretion disk spreads out to the tidal limitation radius and has an extended hot spot or line region. The hot spot or line is hotter than the remaining outer part of the disk in quiescence or in intermediate state, but does not stand out completely from the disk flux in (super)outbursts. Conclusions. We claim that this object represents a link between two distinct classes of SU UMa-type and SW Sex-type cataclysmic variables. The accretion flow structure in the disk corresponds to the SW Sex systems, but the physical conditions inside the disk fit the behaviour of SU UMa-type objects.

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“…The system parameters are quite uncertain. The values listed in Table C1 were taken from , Mennickent et al (2006) and Urban & Sion (2006). Properties of the secondary star are discussed by Mennickent & Diaz (2002), Harrison et al (2009) and Littlefair et al (2000).…”

Section: Appendix B: System Parametersmentioning

confidence: 99%

A comparative study of the strength of flickering in cataclysmic variables

Bruch

2021

Preprint

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Flickering is a universal phenomenon in accreting astronomical systems which still defies detailed physical understanding. It is particularly evident in cataclysmic variables (CVs). Attempting to define boundary conditions for models, the strength of the flickering is measured in several thousand light curves of more than 100 CVs. The flickering amplitude is parameterized by the FWHM of a Gaussian fit to the magnitude distribution of data points in a light curve. This quantity requires several corrections before a comparison between different sources can be made. While no correlations of the flickering strength with simple parameters such as component masses, orbital inclination or period were detected, a dependence on the absolute magnitude of the primary component and on the CV subtype is found. In particular, flickering in VY Scl tpye novalike variables is systematically stronger than in UX UMa type novalikes. The broadband spectrum of the flickering light source can be fit by simple models but shows excess in the U band. When the data permitted to investigate the flickering strength as a function of orbital phase in eclipsing CVs, such a dependence was found, but it is different for different systems. Surprisingly, there are also indications for variations of the flickering strength with the superhump phase in novalike variables with permanent superhumps. In dwarf novae, the flickering amplitude is high during quiescence, drops quickly at an intermediate magnitude when the system enters into (or returns from) an outburst and, on average, remains constant above a given brightness threshold.

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Doppler tomography of the dwarf novae VY Aquari and WX Ceti

Cited by 4 publications

References 26 publications

Time-resolved spectroscopy of the pulsating CV GW Lib

Time-resolved spectroscopy of the pulsating CV GW Lib

The period-gap cataclysmic variable CzeV404 Her: A link between SW Sex and SU UMa systems

A comparative study of the strength of flickering in cataclysmic variables

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