QUIESCENT SUPERHUMPS DETECTED IN THE DWARF NOVA V344 LYRAE BY
                    <i>KEPLER</i>

Still, M.; Howell, Steve B.; Wood, M. A.; Cannizzo, J. K.; Smale, A. P.

doi:10.1088/2041-8205/717/2/l113

Cited by 53 publications

(55 citation statements)

References 31 publications

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“…We estimated this offset visually and it agrees well with a mean amplitude of the quiescent variability depicted in Fig. 1 in Still et al (2010). Therefore, the rms-flux relation of V344 Lyr can still have the typical linear shape, but is somehow deformed due to other variability sources not connected with the accretion process or flickering.…”

Section: Rms-flux Analysissupporting

confidence: 81%

“…The quiescent data were divided into one-day intervals, yielding the low frequency limit approximately log(f /Hz) = −5.0, and every quiescent interval yields an individual PDS. The 2 The period is thought to be an orbital period, but following Still et al (2010) it can also be a negative superhump generated by a retrograde-precessing accretion disc. 3 For a long-term light curves (first 740 days) see Figs.…”

Section: Methodsmentioning

confidence: 99%

“…We selected a light curve subsample with a constant flux level in order to easily transform the original light curve into a "superhumping" light curve using the equation (2) where ψnew is the transformed flux, 0.1×ψorig is the transformation of the original V1504 Cyg flux to get similar fluxes as in the left inset panel of Fig. 1 in Still et al (2010), 0.5×165 is the estimated half amplitude of the superhumps, t is time coordinate in days and t×71.4 is a term to get the same "superhump" period of 2.1 h as in Fig. 1 of Still et al (2010).…”

Section: Rms-flux Analysismentioning

confidence: 99%

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Fast stochastic variability study of two SU UMa systems V1504 Cyg and V344 Lyr observed byKeplersatellite

Dobrotka

Ness

Bajčičáková

2016

Mon. Not. R. Astron. Soc.

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We analysed Kepler data of two similar dwarf novae V344 Lyr and V1504 Cyg in order to study optical fast stochastic variability (flickering) by searching for characteristic break frequencies in their power density spectra. Two different stages of activity were analysed separately, i.e. regular outbursts and quiescence. Both systems show similar behaviour during both activity stages. The quiescent power density spectra show a dominant low break frequency which is also present during outburst with a more or less stable value in V344 Lyr while it is slightly higher in V1504 Cyg. The origin of this variability is probably the whole accretion disc. Both outburst power density spectra show additional high frequency components which we interpret as generated by the rebuilt inner disc that was truncated during quiescence. Moreover, V344 Lyr shows the typical linear rms-flux relation which is strongly deformed by a possible negative superhump variability.

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Section: Rms-flux Analysissupporting

confidence: 81%

Section: Methodsmentioning

confidence: 99%

Section: Rms-flux Analysismentioning

confidence: 99%

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Fast stochastic variability study of two SU UMa systems V1504 Cyg and V344 Lyr observed byKeplersatellite

Dobrotka

Ness

Bajčičáková

2016

Mon. Not. R. Astron. Soc.

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“…We should note, however, recent Kepler observations and high-quality ground-based observations have shown that late-stage superhumps persist longer (one or two outburst cycles) after the termination of the superoutburst (e.g. Still et al 2010;Wood et al 2011;Osaki, Kato 2014;Kato et al 2014b;Kato et al 2014a) in ordinary SU UMa-type dwarf nova with high mass-transfer rates in contrast to textbook descriptions (e.g. Warner 1995).…”

Section: Late-stage Superhumpsmentioning

confidence: 82%

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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“…Still et al (2010) list all objects found in both the input catalogue and the CV catalogue made by Downes et al (2001). Additions to the list of Still et al (2010) were made by Williams et al (2010), Feldmeier et al (2011), Ramsay et al (2012, Scaringi et al (2013a) and Ramsay et al (2014). Howell et al (2013) checked spectroscopically if these objects were indeed CVs.…”

Section: Introductionmentioning

confidence: 99%

The rms–flux relation in accreting white dwarfs: another nova-like variable and the first dwarf nova

Sande¹,

Scaringi²,

Knigge³

2015

Monthly Notices of the Royal Astronomical Society

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We report on the detection of the linear rms-flux relation in two accreting white dwarf binary systems: V1504 Cyg and KIC 8751494. The rms-flux relation relates the absolute root-mean-square (rms) variability of the light curve to its mean flux. The light curves analysed were obtained with the Kepler satellite at a 58.8 s cadence. The rmsflux relation was previously detected in only one other cataclysmic variable, MV Lyr. This result reenforces the ubiquity of the linear rms-flux relation as a characteristic property of accretion-induced variability, since it has been observed in several black hole binaries, neutron star binaries and active galactic nuclei. Moreover, its detection in V1504 Cyg is the first time the rms-flux relation has been detected in a dwarf novatype CV during quiescence. This result, together with previous studies, hence points towards a common physical origin of accretion-induced variability, independent of the size, mass, or type of the central accreting compact object.

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QUIESCENT SUPERHUMPS DETECTED IN THE DWARF NOVA V344 LYRAE BY KEPLER

Cited by 53 publications

References 31 publications

Fast stochastic variability study of two SU UMa systems V1504 Cyg and V344 Lyr observed byKeplersatellite

Fast stochastic variability study of two SU UMa systems V1504 Cyg and V344 Lyr observed byKeplersatellite

WZ Sge-type dwarf novae

The rms–flux relation in accreting white dwarfs: another nova-like variable and the first dwarf nova

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