Detection of Short Fading Episodes in Two Dwarf Novae from VSNET Observations

Katô, Takeo

doi:10.1093/pasj/56.sp1.s55

Cited by 9 publications

(8 citation statements)

References 44 publications

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“…An outburst of this CRTS CV on 2013 June 4 at 17.5 mag was reported by vsnet (Kato 2013a). A light curve showed a prominent single hump feature with a period of 96.9 min.…”

Section: Css/sdss2154+15mentioning

confidence: 63%

Follow Up Observations of SDSS and CRTS Candidate Cataclysmic Variables

Szkody

Everett

Howell

et al. 2014

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We present photometry of 11 and spectroscopy of 35 potential cataclysmic variables from the Sloan Digital Sky Survey, the Catalina Real-Time Transient Survey and vsnet-alerts. The photometry results include quasi-periodic oscillations during the decline of V1363 Cyg, nightly accretion changes in the likely Polar (AM Herculis binary) SDSS J1344+20, eclipses in SDSS J2141+05 with an orbital period of 76±2 min, and possible eclipses in SDSS J2158+09 at an orbital period near 100 min. Time-resolved spectra reveal short orbital periods near 80 min for SDSS J0206+20, 85 min for SDSS J1502+33, and near 100 min for CSS J0015+26, RXS J0150+37, SDSS J1132+62, SDSS J2154+15 and SDSS J2158+09. The prominent He II line and velocity amplitude of SDSS J2154+15 are consistent with a Polar nature for this object, while the lack of this line and a low velocity amplitude argue against this classification for RXS J0150+37. Single spectra of 10 objects were obtained near outburst and the rest near quiescence, confirming the dwarf novae nature of these objects. * Based on observations obtained with the Apache Point Observatory (APO) 3.5-meter telescope, which is owned and operated by the Astrophysical Research Consortium (ARC).

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“…An outburst of this CRTS CV on 2013 June 4 at 17.5 mag was reported by vsnet (Kato 2013a). A light curve showed a prominent single hump feature with a period of 96.9 min.…”

Section: Css/sdss2154+15mentioning

confidence: 63%

Follow Up Observations of SDSS and CRTS Candidate Cataclysmic Variables

Szkody

Everett

Howell

et al. 2014

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“…The 2002 data are, as far as we are aware, the only observations of this superoutburst. The 2003 superoutburst was first reported on May 2 (Kato 2003). The superhump is visible in both the 2002 May 16 light curve at phase ∼−0.45 and the 2003 May 20 light curve at phase ∼−0.2, but is not visible in later data, either because it had faded or because it was at a phase which was not observed.…”

Section: I G H T-c U Rv E M O R P H O L O G Ymentioning

confidence: 93%

“…OU Vir was observed during descent from superoutburst in both 2002and 2003. Mason et al (2002 found that for OU Vir out of eclipse and during quiescence, V = 18.08 and B − V = 0.14, which corresponds to g ∼ 0.2 mJy (Smith et al 2002).…”

Section: I G H T-c U Rv E M O R P H O L O G Ymentioning

confidence: 99%

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ULTRACAM photometry of the eclipsing cataclysmic variable OU Vir

Feline

Dhillon

Marsh

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present high-speed, three-colour photometry of the faint eclipsing cataclysmic variable OU Vir. For the first time in OU Vir, separate eclipses of the white dwarf and bright spot have been observed. We use timings of these eclipses to derive a purely photometric model of the system, obtaining a mass ratio of q = 0.175 +/- 0.025, an inclination of i = 79.2 +/- 0.7 degrees and a disc radius of Rd/a = 0.2315 +/- 0.0150. We separate the white dwarf eclipse from the lightcurve and, by fitting a blackbody spectrum to its flux in each passband, obtain a white dwarf temperature of T = 21700 +/- 1200 K and a distance of D = 650 +/- 210 pc. Assuming that the primary obeys the Nauenberg (1972) mass-radius relation for white dwarfs and allowing for temperature effects, we also find a primary mass Mw/Msun = 0.90 +/- 0.19, primary radius Rw/Rsun = 0.0097 +/- 0.0031 and orbital separation a/Rsun = 0.75 +/- 0.05.Comment: 8 pages LaTeX, 6 figures. Accepted by MNRAS; erratum added at end. Mon.Not.Roy.Astron.Soc. 347 (2004) 1173, erratum in pres

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“…In February 2004, Pojmanski (VSNET-alert 7982) detected the outburst of a new eruptive star in Libra, QZ Lib (aka ASAS 153616-0839.1). 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: 94%

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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Detection of Short Fading Episodes in Two Dwarf Novae from VSNET Observations

Cited by 9 publications

References 44 publications

Follow Up Observations of SDSS and CRTS Candidate Cataclysmic Variables

Follow Up Observations of SDSS and CRTS Candidate Cataclysmic Variables

ULTRACAM photometry of the eclipsing cataclysmic variable OU Vir

The cataclysmic variable QZ Lib: a period bouncer

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