Spectroscopic Classification of Cataclysmic Variable Candidates

Schmidtobreick, L.; Galli, Lorenzo; Whiting, Alan B.; Tappert, C.; Carver, A. J.

doi:10.1086/432671

Cited by 8 publications

(8 citation statements)

References 20 publications

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“…The higher Balmer series lines were instead seen in absorption. Our spectrum differs remarkably from that of Schmidtobreick et al (2005b) because of its low quality. From our S/N we get an upper limit for the EW of not identified lines EW < 5 Å.…”

Section: V888 Cenmentioning

confidence: 56%

“…1 reveals a not very steep hot continuum with only a relatively weak Hα and possible, also weak, Bowen blend emissions superimposed. Schmidtobreick et al (2005b) obtained "the first spectrum of V888 Cen in quiescence" nine years after the outburst. In their spectrum, faint emission lines of Hα, Hβ, and Hγ, as well as He  4686 Å and the Bowen blend, were presented.…”

Section: V888 Cenmentioning

confidence: 99%

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SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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Aims. We report on recent optical observations of the stellar and the nebular remnants of 22 southern post-novae. Methods. In this study, for each of our targets, we obtained and analysed long-slit spectra in the spectral range 3500-6600 Å and inResults. The changes in the emission lines' equivalent widths with the time since the outburst agree with earlier published results of other authors. We estimated an average value α = 2.37 for the exponent of the power law fitted to the post-novae continua. Our observations clearly show the two-component structure of the V842 Cen expanding nebulae, owing to the different velocities of the ejected matter. We discovered an expanding shell around V382 Vel with an outer diameter of about 12 .

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Section: V888 Cenmentioning

confidence: 56%

Section: V888 Cenmentioning

confidence: 99%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

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“…Not much is know about the object. Schmidtobreick et al (2005) measured a spectroscopic orbital period. Modelling UV spectra, Wolfe et al (2013) obtained a primary star mass of roughly 0.6M⊙, and an orbital inclination of no more than 60 o .…”

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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“…Light curves taken worldwide revealed that the object showed periodic variability with a probably increasing period (Kiyota 2004), which was interpreted as growing superhumps with a final period of P sh = 0.06501(3) d (Kato 2004). QZ Lib was then spectroscopically confirmed of being a dwarf nova into outburst by Schmidtobreick et al (2004).…”

Section: Introductionmentioning

confidence: 99%

The cataclysmic variable QZ Lib: a period bouncer

Pala

Schmidtobreick

Tappert

et al. 2018

Monthly Notices of the Royal Astronomical Society

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While highly evolved cataclysmic variables (CVs) with brown dwarf donors, often called "period bouncers", are predicted to make up 40 − 70% of the Galactic CV population, only a handful of such systems are currently known. The identification and characterization of additional period bouncers is therefore important to probe this poorly understood phase of CV evolution. We investigate the evolution of the CV QZ Lib following its 2004 super-outburst using multi-epoch spectroscopy. From time-resolved spectroscopic observations we measure the orbital period of the system, P orb = 0.06436(20) d, which, combined with the superhump period P SH = 0.064602(24) d, yields the system mass ratio, q = 0.040(9). From the analysis of the spectral energy distribution we determine the structure of the accretion disc and the white dwarf effective temperature, T eff = 10 500 ± 1500 K. We also derive an upper limit on the effective temperature of the secondary, T eff 1700 K, corresponding to a brown dwarf of T spectral type. The low temperature of the white dwarf, the small mass ratio and the fact that the donor is not dominating the near-infrared emission are all clues of a post bounce system. Although it is possible that QZ Lib could have formed as a white dwarf plus a brown dwarf binary, binary population synthesis studies clearly suggest this scenario to be less likely than a period bouncer detection and we conclude that QZ Lib is a CV that has already evolved through the period minimum.

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Spectroscopic Classification of Cataclysmic Variable Candidates

Cited by 8 publications

References 20 publications

SALT observations of southern post-novae

SALT observations of southern post-novae

A comparative study of the strength of flickering in cataclysmic variables

The cataclysmic variable QZ Lib: a period bouncer

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