THE<i>KEPLER</i>LIGHT CURVE OF V344 Lyrae: CONSTRAINING THE THERMAL-VISCOUS LIMIT CYCLE INSTABILITY

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

doi:10.1088/0004-637x/725/2/1393

Cited by 69 publications

(96 citation statements)

References 70 publications

(91 reference statements)

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“…Cannizzo et al (2010) reported that the fading rates of WZ Sge is much faster than the Kepler objects, V344 Lyr and V1504 Cyg, and suggested that this different could arise from the strong dependence of the viscosity in quiescence. Cannizzo et al (2010) interpreted that smaller viscosity in quiescence gives rise to a larger surface density at the start of the superoutburst and hence a steeper viscous decay. His analysis, however, used different segments between ordinary SU UMa-type dwarf novae (linearly fading part) and WZ Sge (initial rapid fading).…”

Section: Properties Of Rebrighteningsmentioning

confidence: 99%

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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Section: Properties Of Rebrighteningsmentioning

confidence: 99%

WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

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“…Although there have been claims of other mechanisms [the enhanced mass-transfer model (Smak 1991) and pure thermal instability model (Cannizzo et al 2010)], it has been demonstrated using Kepler observations of V1504 Cyg and V344 Lyr that the TTI model is the best one to explain the observations ) (see also Osaki, Kato 2014).…”

Section: Introductionmentioning

confidence: 99%

Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015–2016)

Katô

Hambsch

Monard

et al. 2016

Publications of the Astronomical Society of Japan

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Continuing the project described by Kato et al. (2009), we collected times of superhump maxima for 128 SU UMa-type dwarf novae observed mainly during the 2015-2016 season and characterized these objects. The data have improved the distribution of orbital periods, the relation between the orbital period and the variation of superhumps, the relation between period variations and the rebrightening type in WZ Sge-type objects. Coupled with new measurements of mass ratios using growing stages of superhumps, we now have a clearer and statistically greatly improved evolutionary path near the terminal stage of evolution of cataclysmic variables. Three objects (V452 Cas, KK Tel, ASASSN-15cl) appear to have slowly growing superhumps, which is proposed to reflect the slow growth of the 3:1 resonance near the stability border. ASASSN-15sl, ASASSN-15ux, SDSS J074859.55+312512.6 and CRTS J200331.3−284941 are newly identified eclipsing SU UMa-type (or WZ Sge-type) dwarf novae. ASASSN-15cy has a short (∼0.050 d) superhump period and appears to belong to EI Psc-type objects with compact secondaries having an evolved core. ASASSN-15gn, ASASSN-15hn, ASASSN-15kh and ASASSN-16bu are candidate period bouncers with superhump periods longer than 0.06 d. We have newly obtained superhump periods for 79 objects and 13 orbital periods, including periods from early superhumps. In order that the future observations will be more astrophysically beneficial and rewarding to observers, we propose guidelines how to organize observations of various superoutbursts.

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“…Cannizzo et al (2010) studied the systematics of outbursts in V344 Lyr. Wood et al (2011) analyzed the positive and negative superhumps in the same object.…”

Section: Introductionmentioning

confidence: 99%

“…where P h is the orbital period in hr, α hot, −1 = α hot /0.1, and Cannizzo et al 2010). Cannizzo et al (2010) studied the Kepler light curves of V344 Lyr and V1504 Cyg and compared the slow fading rate during the superoutburst with other SU UMa-type dwarf novae.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Survey of period variations of superhumps in SU UMa-type dwarf novae. V. The fifth year (2012–2013)

Katô¹,

Hambsch²,

Maehara³

et al. 2014

Publications of the Astronomical Society of Japan

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Continuing the project described in Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for SU UMa-type dwarf novae mainly observed during the 2012-2013 season. We found three objects (V444 Peg, CSS J203937, and MASTER J212624) having strongly positive period derivatives despite the long orbital period (P orb ). By using the period of growing stage (stage A) superhumps, we obtained mass ratios for six objects. We characterized nine new WZ Sge-type dwarf novae. We made a pilot survey of the decline rate in the slowly fading parts of SU UMa-type and WZ Sge-type outbursts. The decline time scale was found to generally follow an expected P 1/4 orb dependence, and WZ Sge-type outbursts also generally follow this trend. There are some objects which show slower decline rates, and we consider these objects good candidates for period bouncers. We also studied unusual behavior in some objects, including BK Lyn which made a transition from an ER UMa-type state to a novalike (standstill) state in 2013, and unusually frequent occurrences of superoutbursts in NY Ser and CR Boo. We applied the least absolute shrinkage and selection operator (Lasso) power spectral analysis, which has been proven to be very effective in analyzing the Kepler data, to the ground-based photometry of BK Lyn, and detected a dramatic disappearance of the signal of negative superhumps in 2013. We suggested that the mass-transfer rates did not strongly vary between the ER UMa-type state and novalike state in BK Lyn, and this transition was less likely caused by a systematic variation of the mass-transfer rate.

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THEKEPLERLIGHT CURVE OF V344 Lyrae: CONSTRAINING THE THERMAL-VISCOUS LIMIT CYCLE INSTABILITY

Cited by 69 publications

References 70 publications

WZ Sge-type dwarf novae

WZ Sge-type dwarf novae

Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015–2016)

Survey of period variations of superhumps in SU UMa-type dwarf novae. V. The fifth year (2012–2013)

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