Characteristics of High-State/Low-State Transitions in VY Sculptoris Stars

Honeycutt, R. K.; Kafka, S.

doi:10.1086/422737

Cited by 58 publications

(64 citation statements)

References 50 publications

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“…The term "nova-like variable" includes all non-eruptive cataclysmic variables (CVs) for which the accretion disc is believed to be permanently in the high-viscosity state associated with dwarf nova outbursts. The VY Scl stars are a small subset of these which occasionally undergo a drop in flux to a low state (Leach et al 1999;Honeycutt & Kafka 2004). These low states can last for several hundred days and are believed to be caused by intervals of low mass-transfer in the system.…”

Section: Introductionmentioning

confidence: 99%

X-ray and UV observations of V751 Cygni in an optical high state

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Osborne

Beardmore

et al. 2014

A&A

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Aims. The VY Scl system (anti-dwarf nova) V751 Cyg is examined following a claim of a super-soft spectrum in the optical low state. Methods. A serendipitous XMM-Newton X-ray observation and, 21 months later, Swift X-ray and UV observations, have provided the best such data on this source so far. These optical high-state datasets are used to study the flux and spectral variability of V751 Cyg.Results. Both the XMM-Newton and Swift data show evidence for modulation of the X-rays for the first time at the known 3.467 h orbital period of V751 Cyg. In two Swift observations, taken ten days apart, the mean X-ray flux remained unchanged, while the UV source brightened by half a magnitude. The X-ray spectrum was not super-soft during the optical high state, but rather due to multi-temperature optically thin emission, with significant (10 21−22 cm −2 ) absorption, which was higher in the observation by Swift than that of XMM-Newton. The X-ray flux is harder at orbital minimum, suggesting that the modulation is related to absorption, perhaps linked to the azimuthally asymmetric wind absorption seen previously in Hα.

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Section: Introductionmentioning

confidence: 99%

X-ray and UV observations of V751 Cygni in an optical high state

Page

Osborne

Beardmore

et al. 2014

A&A

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“…This seems unlikely, for two reasons. First, the long-term light curves of VY Scl stars tend to look quite different from those of dwarf novae-VY Scl stars typically remain in a high state for months or years, and only occasionally fade by large amounts, up to 5 mag (see examples in Honeycutt & Kafka 2004). The light curve here, by contrast, consists of frequent, moderate-amplitude outbursts from a faint state.…”

Section: Discussionmentioning

confidence: 87%

The Eclipsing Cataclysmic Variable Lanning 386: Dwarf Nova, SW Sextantis Star, or Both?

Brady

Thorstensen

Koppelman

et al. 2008

PUBL ASTRON SOC PAC

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ABSTRACT. We present photometry and spectroscopy of the suspected cataclysmic variable (CV) Lanning 386. We confirm that it is a CV, and observe deep eclipses, from which we determine the orbital period P orb to be 0:1640517 AE 0:0000001 days (¼ 3:94 h). Photometric monitoring over two observing seasons shows a very active system with frequent outbursts of variable amplitude, up to ∼2 mag. The spectrum in quiescence is typical of dwarf novae, but in its high state the system shows strong He II emission and a broad C IV Wolf-Rayet feature. This is unusual for dwarf novae in outburst and indicates a high excitation. In its high state the system shows some features reminiscent of an SW Sextantis-type CV, but lacks others. We discuss the classification of this puzzling object.

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“…This further supports that LQ Peg is a nova-like CV. Honeycutt and Kafka (2004) give a light curve from 1993 to 2003. It shows that LQ Peg spends most of its time in the high state, as VY Scl stars do.…”

Section: Introductionmentioning

confidence: 99%

The photometric periods of the nova-like cataclysmic variable LQ Pegasi (PG 2133+115)

Rude

Ringwald

2012

New Astronomy

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We present a time-resolved differential photometric study and time series analysis of the nova-like cataclysmic variable star LQ Peg. We discover three periodicities in the photometry, one with a period of 3.42 ± 0.03 hours, and another with a period of 56.8 ± 0.01 hours. We interpret these to be the apsidal superhump and precessional periods of the accretion disk, respectively, and predict that the orbital period of LQ Peg is 3.22 ± 0.03 hours. The third periodicity, with a period of 41.3 ± 0.01 hours, we interpret to be the nodal precessional period of the accretion disk. We also report a flare that lasted four minutes and had an energy in visible light of (1.2 ± 0.3) × 10 36 ergs, or 10 4-5 times more energetic than the largest solar flares, comparable to the most energetic visible-light stellar flares known. We calculate the absolute magnitude of LQ Peg to be M J = 4.78 ± 0.54, and its distance to be 800 ± 200 pc.

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Characteristics of High-State/Low-State Transitions in VY Sculptoris Stars

Cited by 58 publications

References 50 publications

X-ray and UV observations of V751 Cygni in an optical high state

X-ray and UV observations of V751 Cygni in an optical high state

The Eclipsing Cataclysmic Variable Lanning 386: Dwarf Nova, SW Sextantis Star, or Both?

The photometric periods of the nova-like cataclysmic variable LQ Pegasi (PG 2133+115)

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