V344 LYRAE: A TOUCHSTONE SU UMa CATACLYSMIC VARIABLE IN THE KEPLER FIELD

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

doi:10.1088/0004-637x/741/2/105

Cited by 92 publications

(134 citation statements)

References 81 publications

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“…Many well-observed SU UMa-type dwarf novae, including Kepler observations of V585 Lyr , have been confirmed show continuous O −C diagrams (no phase jump) and the appearance of superhumps with ∼0.5 phase shift is only limited to high masstransfer systems [e.g. V344 Lyr (Wood et al 2011), YZ Cnc ), V1159 Ori ), VW Hyi (van der Woerd et al 1988]. This observation is in line with the classical interpretation that late superhumps arise from the hot spot on an elliptical disk (Osaki 1985).…”

Section: Late-stage Superhumpsmentioning

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: Late-stage Superhumpsmentioning

confidence: 99%

WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

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“…an analysis of the Kepler data of V344 Lyr by Wood et al 2011). In most cases they appear in quiescence and sometimes can survive a normal outburst (Wood et al 2011;Osaki & Kato 2013). However, in rare cases more complete radial velocity data set is desirable to confirm this reasoning.…”

Section: Orbital Period Determinationmentioning

confidence: 99%

The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

Neustroev

Marsh

Zharikov

et al. 2017

Mon. Not. R. Astron. Soc.

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We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7−311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d and a very gentle decline with a rate of 0.02 mag d −1 , and it displayed an extended post-outburst decline lasting at least 500 d. Simultaneously with the start of the rapid fading from the superoutburst plateau, the system showed the appearance of a strong near-infrared excess resulting in very red colours, which reached extreme values (B − I ≃ 1.4) about 20 d later. The colours then became bluer again, but it took at least 250 d to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 d after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess 0.8 per cent, indicating a very low mass ratio q 0.045. With such a small mass ratio the donor mass should be below the hydrogen-burning minimum mass limit. The observed infrared flux in quiescence is indeed much lower than is expected from a cataclysmic variable with a nearmain-sequence donor star. This strongly suggests a brown-dwarf-like nature for the donor and that SSS J122221.7−311525 has already evolved away from the period minimum towards longer periods, with the donor now extremely dim.

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“…Secondary maxima of superhumps are relatively prominent in this system and became stronger than the original maxima during the later course of the superoutburst. The same feature was recorded in the Kepler data of V344 Lyr, which was considered to arise from the accretion stream resulting a bright spot that sweeps around the rim of the non-axisymmetric disk (Wood et al 2011). The maxima for E ≥97 in table 9 correspond to these secondary maxima, and are excluded for obtaining the period in table 3.…”

Section: V1040 Centaurimentioning

confidence: 94%

“…The maxima for E ≥97 in table 9 correspond to these secondary maxima, and are excluded for obtaining the period in table 3. The interpretation in Wood et al (2011) would suggest a high mass-transfer rate, and indeed "traditional" late superhumps with an ∼0.5 phase jump are seen only in systems with frequent outbursts (e.g. Kato et al 2013a).…”

Section: V1040 Centaurimentioning

confidence: 98%

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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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V344 LYRAE: A TOUCHSTONE SU UMa CATACLYSMIC VARIABLE IN THE KEPLER FIELD

Cited by 92 publications

References 81 publications

WZ Sge-type dwarf novae

WZ Sge-type dwarf novae

The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

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

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