High-speed photometry of faint cataclysmic variables - I. V359 Cen, XZ Eri, HY Lup, V351 Pup, V630 Sgr, YY Tel, CQ Vel and CE-315

Woudt, P. A.; Warner, Brian D.

doi:10.1046/j.1365-8711.2001.04857.x

Cited by 56 publications

(47 citation statements)

References 38 publications

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“…This identification confirms the quiescent magnitude (V = 18.7) reported by Woudt & Warner (2001). The quiescent magnitudes (21 or V fainter than 20.5) reported by Duerbeck (1987) and Munari & Zwitter (1998) seem to be underestimated.…”

Section: Observationssupporting

confidence: 88%

“…This observation, on the contrary to the suggestion by Woudt & Warner (2001), indicates that the superhumps or late superhumps in V359 Cen must have decayed more rapidly, as in other usual SU UMatype dwarf novae (see Kato et al 2001a for a recent example of the decay of late superhumps). V359 Cen is thus unlikely related to WZ Sge-type dwarf novae which always show long persistence of late superhumps.…”

Section: Superhump Excess and Late Superhumpscontrasting

confidence: 67%

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The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

Katô

Stubbings²,

Nelson

et al. 2002

A&A

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Abstract. We detected four outbursts of V359 Cen (possible nova discovered in 1939) between 1999 and 2002. Time-resolved CCD photometry during two outbursts (1999 and 2002) revealed that V359 Cen is actually a long-period SU UMa-type dwarf nova with a mean superhump period of 0.08092(1) d. We identified its supercycle length as 307-397 d. This secure identification of the superhump period precludes the previously supposed possibility that V359 Cen could be related to a WZ Sge-type system with a long persistence of late superhumps. The outburst characteristics of V359 Cen are, however, rather unusual in its low occurrence of normal outbursts.

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Section: Observationssupporting

confidence: 88%

Section: Superhump Excess and Late Superhumpscontrasting

confidence: 67%

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

Katô

Stubbings²,

Nelson

et al. 2002

A&A

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“…In such a pre-whitened data set we did not find any significant periodicity (in a range of 0.05-0.5 days). However, we cannot completely rule out that V630 Sgr is a permanent superhumper as Woudt & Warner (2001) suggest. Possibly, the number and cadence of observations in this case is too poor for a robust detection of low-amplitude superhumps.…”

Section: V630 Sgr Was Discovered By Sigeki Okabayasi In 1936mentioning

confidence: 79%

Ogle Atlas of Classical Novae. I. Galactic Bulge Objects

Mróz

Udalski

Poleski

et al. 2015

ApJS

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Eruptions of classical novae are possible sources of lithium formation and gamma-ray emission. Nova remnants can also become Type Ia supernovae (SNe Ia). The contribution of novae to these phenomena depends on nova rates, which are not well established for the Galaxy. Here, we directly measure a Galactic bulge nova rate of 13.8 ± 2.6 yr −1 . This measurement is much more accurate than any previous measurement of this kind thanks to many years' monitoring of the bulge by the Optical Gravitational Lensing Experiment (OGLE) survey. Our sample consists of 39 novae eruptions, ∼1/3 of which are OGLE-based discoveries. This long-term monitoring allows us to not only measure the nova rate but also to study in detail the light curves of 39 eruptions and more than 80 post-nova candidates. We measured orbital periods for 9 post-novae and 9 novae, and in 14 cases we procured the first estimates. The OGLE survey is very sensitive to the frequently erupting recurrent novae. We did not find any object similar to M31 2008-12a, which erupts once a year. The lack of detection indicates that there is only a small number of them in the Galactic bulge.

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“…V359 Cen: The object is a well-confirmed ordinary SU UMa-type dwarf nova (Kato et al 2002a;Woudt, Warner 2001;Kato et al 2009a;Kato et al 2014a).…”

Section: Current Status Of Candidates Inmentioning

confidence: 94%

WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

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We have summarized the current understanding and recently obtained findings about WZ Sge-type dwarf novae. We also reviewed the historical development of the understanding of these objects, provided the modern criteria, and reviewed the past research in relation to superhumps, early superhumps and the outburst mechanism. We regard that the presence of early superhumps (reflecting the 2:1 resonance) and long or multiple rebrightenings are the best distinguishing properties of WZ Sge-type dwarf novae. We provided the updated list of nearly 100 WZ Sge-type dwarf novae mainly based on the data obtained by the VSNET Collaboration up to Kato et al. (2015) and discussed the statistics. We could detect early superhumps with amplitude larger than 0.02 mag in 63% of the studied WZ Sge-type dwarf novae, which makes early superhumps a useful distinguishing feature for WZ Sge-type dwarf novae. Theoretical light curves of early superhumps generally appear to reproduce the existence of many low-amplitude objects, supporting the geometrical origin of early superhumps. Using the recently developed method of measuring mass ratios using developing phase of superhumps (stage A superhumps), we showed that there is a linear relation between the period variation of superhumps and the mass ratio in WZ Sge-type objects. By using this relation, we were able to draw an evolutionary picture of a large number of WZ Sge-type and identified the type of outburst to be an evolutionary sequence: type C → D → A → B → E, with some outliers for type-B objects. The duration of stage A (evolutionary phase) of superhumps is also well correlated with the estimated mass ratios. By using mass ratios from stage A superhumps and durarion of stage A, we have been able to identify best candidates for period bouncers.

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High-speed photometry of faint cataclysmic variables - I. V359 Cen, XZ Eri, HY Lup, V351 Pup, V630 Sgr, YY Tel, CQ Vel and CE-315

Cited by 56 publications

References 38 publications

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

Ogle Atlas of Classical Novae. I. Galactic Bulge Objects

WZ Sge-type dwarf novae

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