Survey of period variations of superhumps in SU UMa-type dwarf novae. VI. The sixth year (2013–2014)

Katô, Takeo; Dubovský, Pavol A.; Kudzej, Igor; Hambsch, Franz-Josef; Miller, Ian; Ohshima, Tomohito; Nakata, Chikako; Kawabata, Miho; Nishino, Hirochika; Masumoto, Kazunari; Mizoguchi, Shigeru; Yamanaka, Masahito; Matsumoto, Katsura; Sakai, Daisuke; Fukushima, Daiki; Matsuura, M.; Bouno, Genki; Takenaka, Mikihito; Shinichi, Nakagawa; Iino, Eriko; Pickard, R.; Maeda, Yutaka; Henden, A. A.; Kasai, Kiyoshi; Kiyota, S.; Akazawa, Hidehiko; Imamura, Kazuyoshi; Miguel, Enrique de; Maehara, Hiroyuki; Monard, B.; Павленко, Е. П.; Antonyuk, K. A.; Pit, N.; Antonyuk, Oksana I.; Baklanov, A. V.; Ruiz, Javier; Richmond, M.; Oksanen, A.; Harlingten, C.; Shugarov, S. Yu.; Chochol, D.; Nocentini, Francesca; Schmeer, P.; Bolt, Greg; Nelson, Peter; Ulowetz, Joseph; Sabo, Richard; Goff, W.; Stein, William; Michel, R.; Dvorak, Shawn; Voloshina, I.; Metlov, V. G.; Katysheva, N. A.; Neustroev, V.; Sjoberg, George; Dębski, B.; Sowicka, Paulina; Klimaszewski, Marcin; Curyło, M.; Morelle, Etienne; Curtis, Ivan A.; Iwamatsu, H.; Butterworth, N.; Андреев, М. В.; Parakhin, N.; Sklyanov, A. S.; Shiokawa, Kazuhiko; Novák, Rudolf; Irsmambetova, T. R.; Itoh, Hiroshi; Ito, Y.; Hirosawa, Kenji; Денисенко, Д.; Kochanek, C. S.; Shappee, B. J.; Stanek, K. Z.; Prieto, J. L.; Itagaki, K.; Stubbings, Rod; Ripero, José; Muyllaert, Eddy; Poyner, G.

doi:10.1093/pasj/psu072

Cited by 43 publications

(10 citation statements)

References 137 publications

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“…Superoutbursts had amplitudes of ∼ 5 mag and lasted longer than ∼ 10 days (RG05). Superhumps, with 𝑃 sh 1.484 hr, were observed approximately 1 day after superoutburst maximum, and Kato et al (2014𝑏) noted that the superhump profile in the light curves of a 2013 superoutburst became double-humped during the rapid fading phase.…”

Section: V521 Pegmentioning

confidence: 99%

Transient behaviour of three SU UMa-type dwarf novae: AR Pic, QW Ser, and V521 Peg

Szegedi

Charles

Meintjes

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Changes in the supercycle lengths of some SU UMa-type dwarf novae have been detected by other studies, and indicate that the mass transfer rates noticeably decrease over time. We investigated the supercycle lengths of three SU UMa-type dwarf novae: AR Pic, QW Ser, and V521 Peg, to determine if they have detectable changes in their supercycles. We present the results of optical spectroscopic and photometric observations of these sources. Our observations were conducted in 2016 and 2017 at the Boyden Observatory and the Sutherland station of the South African Astronomical Observatory. The quiescent results indicated that all three sources are typical SU UMa-type dwarf novae. We also present results of AR Pic and QW Ser in outburst and of V521 Peg during a precursor outburst and superoutburst. Light curves were supplemented by the Catalina Real-Time Transient Survey, the ASAS-3 and ASAS-SN archives, and the AAVSO International Database in order to investigate the long-term behaviour of these sources. Our results combined with catalogued properties for all short-period dwarf novae show a possible relationship between the supercycle time in SU UMa systems and their orbital periods, which is interpreted as the decline in the mass transfer rate as systems evolve towards and away from the ‘period minimum’. At the shortest orbital periods, SU UMa systems are almost indistinguishable from WZ Sge systems. However, we propose that the scaleheight between the secondary’s photosphere and L1 may be a factor that distinguish the SU UMa subclasses.

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Section: V521 Pegmentioning

confidence: 99%

Transient behaviour of three SU UMa-type dwarf novae: AR Pic, QW Ser, and V521 Peg

Szegedi

Charles

Meintjes

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…A peculiar narrow emission line within the double-peaked Hα line was also observed, which is ascribed to chromospheric emission from the irradiated inner hemisphere of the donor. Kato et al (e.g [36] and [37]) observed superoutbursts in 2012 and 2013. To date no normal outbursts have been observed for this source.…”

Section: V521 Pegmentioning

confidence: 99%

Transient emission of selected CRTS Cataclysmic Variables

Szegedi¹,

Odendaal²,

Meintjes³

et al. 2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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We present optical photometric and spectroscopic observations of three SU UMa-type dwarf novae, i.e. AR Pic, QW Ser and V521 Peg, conducted in 2016 and 2017. These sources were selected from the Catalina Real-Time Transient Survey and observed during quiescence, outburst (AR Pic and QW Ser) and superoutburst (V521 Peg). For AR Pic, strong flickering in the light curves and an asymmetric double-peaked Hβ emission line in the spectra, confirmed the presence of a very active hot spot. During outburst, detected on 18 February 2017, it exhibited a ∼ 3.3 magnitude brightening. The projected velocity of the inner edge of the accretion disc is ∼ 2000 km s −1. An outburst of QW Ser was detected on 8 August 2016. Absorption lines, characteristic of an optically thick disc during outburst, were detected and an outflow velocity of ∼ 1000 km s −1 was determined. Optical spectra during the superoutburst of V521 Peg were obtained for the first time, confirming the superoutburst nature of the outburst, as also observed in other SU UMa-type dwarf novae. The superoutburst was detected on 1 September 2017. Welldefined superhumps were observed, with an average superhump period of P sh ∼ 1.48 hr. A mass ratio of q ∼ 0.14 was determined from the period excess of ε ∼ 3%.

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“…The times of all observations were corrected to barycentric Julian Days (BJD). The data were analyzed in the same way as described in [15] and [16]. Figure 1 shows the general light curves of the 2013 (upper panel) and 2016 (lower panel) observations, including six supercycles and three complete supercycles, respectively.…”

Section: Observations and Analysismentioning

confidence: 99%

The bridge between ER Ursae Majoris-type dwarf nova and nova-like system

Ishioka¹,

Katô²

2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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We report on the photometric observation of RZ LMi, which is a dwarf nova renowned for its extremely short ( 19 d) and regular supercycle, in 2013 and 2016. The supercycles observed in both years were longer than previously reported values of 19 d. Especially in 2016, we observed two exceptionally long superoutbursts with drations of 28 d and 48 d, which require very high mass transfer rate, 97 % and 99 % of the critical mass transfer rate, respectively. We consider that the object virtually experienced a transition to the nova-like state. We detected growing (stage A) superhumps with a mean period of 0.0602(1) d in 2013 and 2016, and possible negative superhumps with a period of 0.05710(1) d. By using the two periods, we estimated an orbital period of 0.05792 d. The orbital period suggests a mass ratio of 0.10, which is larger than mass ratios in WZ Sge-type dwarf novae with orbital periods similar to RZ LMi, and even above that of some ordinary SU UMa-type dwarf novae with similar orbital periods. The exceptionally high mass-transfer rate in this object may possibly be ecplained by a stripped secondary with an evolved core in a system evolving toward an AM CVn-type object.

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Survey of period variations of superhumps in SU UMa-type dwarf novae. VI. The sixth year (2013–2014)

Cited by 43 publications

References 137 publications

Transient behaviour of three SU UMa-type dwarf novae: AR Pic, QW Ser, and V521 Peg

Transient behaviour of three SU UMa-type dwarf novae: AR Pic, QW Ser, and V521 Peg

Transient emission of selected CRTS Cataclysmic Variables

The bridge between ER Ursae Majoris-type dwarf nova and nova-like system

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