Discovery of a New Dwarf Nova, TSS J022216.4+412259.9: WZ Sge-Type Dwarf Nova Breaking the Shortest Superhump Period Record

Imada, Akira; Kubota, Kaori; Katô, Takeo; Nogami, Daisaku; Maehara, Hiroyuki; Nakajima, Kazuhiro; Ishioka, Makoto Uemura Ryoko

doi:10.1093/pasj/58.4.l23

Cited by 42 publications

(37 citation statements)

References 28 publications

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“…The origin of unique light variations, as well as their evolutionary status, are still in debate (e.g., Osaki, Meyer 2003;Nakata et al 2014; see Kato 2015 for a review). Their observational properties are that (1) the amplitude of the superoutburst is large, exceeding ∼ 6 mag (Howell et al 1995), (2) the interval between the successive superoutbursts (supercycle) is unusually long, typically with a time scale of decades (Kato et al 2001), (3) modulations with double-peaked profiles called early superhumps are observed in the early phase of the superoutburst (Kato 2002), and (4) after the end of the plateau stage, single or multiple rebrightenings are observed (Imada et al 2006). Among them, properties (3) and (4) are considered to be unique to WZ Sge-type dwarf novae and to be the defining characteristics (see Kato 2015).…”

Section: Introductionmentioning

confidence: 99%

Unexpected superoutburst and rebrightening of AL Comae Berenices in 2015

Kimura¹,

Katô²,

Imada³

et al. 2016

Publications of the Astronomical Society of Japan

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In 2015 March, the notable WZ Sge-type dwarf nova AL Com exhibited an unusual outburst with a recurrence time of ∼1.5 yr, which is the shortest interval of superoutbursts among WZ Sge-type dwarf novae. Early superhumps in the superoutburst light curve were absent, and a precursor was observed at the onset of the superoutburst for the first time in WZ Sge-type dwarf novae. The present superoutburst can be interpreted as a result of the condition that the disk radius barely reached the 3:1 resonance radius, but did not reach the 2:1 resonance one. Ordinary superhumps immediately grew following the precursor. The initial part of the outburst is indistinguishable from those of superoutbursts of ordinary SU UMa-type dwarf novae. This observation supports the interpretation that the 2:1 resonance suppresses a growth of ordinary superhumps. The estimated superhump period and superhump period derivative are P sh = 0.0573185(11) d and P dot = +1.5(3.1) × 10 −5 , respectively. These values indicate that the evolution of ordinary superhumps is the same as that in past superoutbursts with much larger extent. Although the light curve during the plateau stage was typical for an SU UMa-type dwarf nova, this superoutburst showed a rebrightening, together with a regrowth of the superhumps. The overall light curve of the rebrightening was the almost the same as those observed in previous rebrightenings. This implies that the rebrightening type is inherent in the system.

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Section: Introductionmentioning

confidence: 99%

Unexpected superoutburst and rebrightening of AL Comae Berenices in 2015

Kimura¹,

Katô²,

Imada³

et al. 2016

Publications of the Astronomical Society of Japan

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“…According to Hiroi et al (2009), this difference can be understood as the presence of the mass reservoir, which are the outer gas of the accretion disk and will result in the mass donor for rebrightenings (Kato et al 1998). As V455 And also did not show any rebrightenings along with GW Lib (Type-D rebrightening; Kato et al 2009;Imada et al 2006), this interpretation still holds among V455 And, GW Lib and WZ Sge.…”

Section: The Time Evolution Of Spectramentioning

confidence: 91%

Spectroscopic Observations of V455 Andromedae Superoutburst in 2007: the Most Exotic Spectral Features in Dwarf Nova Outbursts

Tampo,

Nogami,

Kato

et al. 2022

Preprint

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We present our spectroscopic observations of V455 Andromedae during the 2007 superoutburst. Our observations cover this superoutburst from around the optical peak of the outburst to the post-superoutburst stage. During the early superhump phase, the emission lines of Balmer series, He I, He II, Bowen blend, and C IV / N IV blend were detected. He II 4686 line exhibited a double-peaked emission profile, where Balmer emission lines were single-peaked, which is unexpected from its high inclination. In the ordinary superhump phase, Balmer series

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“…Rebrightenings or echo outbursts are one of most striking characteristics of WZ Sge objects. Imada et al (2006) suggested to classify all detected rebrightenings in following 4 types:…”

Section: Phenomenon Of Rebrighteningsmentioning

confidence: 99%

Superhumps in SU UMA Dwarf Novae

Voloshina¹

2018

Proceedings of Accretion Processes in Cosmic Sources — PoS(APCS2016)

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Dwarf novae belong to the class of cataclysmic variables and represent the close binary systems in the late evolutionary stages. They consist of a white dwarf and a red dwarf which fills its Roche lobe and transfers mass to the white dwarf. The gas stream flows from the secondary to the primary white dwarf forming an accretion disk around it. Dwarf novae undergo outburst in semi-periodic intervals of time, when the brightness increases by 3 m to 5 m. For most of them, the faint state (or quiescence) is a normal state. There are 3 types of dwarf novae: U Gem, Z Cam and SU UMa. The last ones have orbital periods about 80 − 180 min, mass of the secondary 3 times less or even more than white dwarf mass. Two types of outbursts are observed in these systems: frequent normal outbursts and superoutbursts which last longer and rise to slightly higher luminosities. During superoutburst they exhibit so-called "superhumps",-brightness increase on the small part of the light curve repeated with the period a few percents longer than the orbital one and amplitude of ∼ 0.1 m − 0.3 m. Superhumps are the most striking phenomenon which exhibited SU UMa dwarf novae and make them interesting and promising objects for study. According to the tidal-thermal model (Osaki, 1996) superhumps are due to gravitational disturbances from the secondary. These disturbances became most effective then the matter of accretion disk reach the 3:1 resonance of the orbital motion of the secondary. The beating of the orbital and precessional periods cause periodic variations, identified as superhumps. Positive and negative superhumps are described. The evolution of superhumps is considered together with the changes of superhump period during the outburst.The observational properties of SU UMa stars are collected by * Speaker. † A footnote may follow.

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Discovery of a New Dwarf Nova, TSS J022216.4+412259.9: WZ Sge-Type Dwarf Nova Breaking the Shortest Superhump Period Record

Cited by 42 publications

References 28 publications

Unexpected superoutburst and rebrightening of AL Comae Berenices in 2015

Unexpected superoutburst and rebrightening of AL Comae Berenices in 2015

Spectroscopic Observations of V455 Andromedae Superoutburst in 2007: the Most Exotic Spectral Features in Dwarf Nova Outbursts

Superhumps in SU UMA Dwarf Novae

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