The 2006 November Outburst of EG Aquarii: the SU UMa Nature Revealed

Imada, Akira; Stubbings, Rod; Katô, Takeo; Uemura, Makoto; Krajci, Thomas; Torii, K.; Sugiyasu, Kei; Kubota, Kaori; Moritani, Yuuki; Ishioka, Ryoko; Kiyota, S.; Monard, L. A. G.; Maehara, Hiroyuki; Nakajima, Kazuhiro; Arai, Akira; Ohsugi, T.; Yamashita, Takuya; Kawabata, Koji S.; Nagae, Osamu; Chiyonobu, Shingo; Fukazawa, Yasushi; Mizuno, T.; Takahashi, H.; Ueda, Atsushi; Hayashi, Tetsutaro; Yoshida, Michitoshi; Yanagisawa, K.; Sato, Shuji; Kino, Motoki; Kitagawa, Masahiro; Sadakane, Kozo; Nogami, Daisaku

doi:10.1093/pasj/60.5.1151

Cited by 8 publications

(2 citation statements)

References 37 publications

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“…CSS 2325−08, or CSS 080101:232519−081819, is one of the first CVs to be found in the CSS survey and was a rediscovery of the known dwarf nova EG Aqr. Imada et al (2008) observed a superoutburst in EG Aqr in 2006 November and found a superhump period of 113.51 min. We observed EG Aqr at a quiescence brightness of r ∼ 19.3 in 2008 October; the details are given in Table 1 and the light curves in Fig.…”

Section: Eg Aqr (Css 080101:232519−081819)mentioning

confidence: 98%

High-speed photometry of faint cataclysmic variables - VII. Targets selected from the Sloan Digital Sky Survey and the Catalina Real-time Transient Survey

Woudt

Warner

Budè

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present high‐speed photometric observations of 20 faint cataclysmic variables (CVs) selected from the Sloan Digital Sky Survey (SDSS) and Catalina catalogues. Measurements are given of 15 new directly measured orbital periods, including four eclipsing dwarf novae (SDSS 0904+03, CSS 0826−00, CSS 1404−10 and CSS 1626−12), two new polars (CSS 0810+00 and CSS 1503−22) and two dwarf novae with superhumps in quiescence (CSS 0322+02 and CSS 0826−00). Whilst most of the dwarf novae presented here have periods below 2 h, SDSS 0805+07 and SSS 0617−36 have relatively long orbital periods of 5.489 and 3.440 h, respectively. The double‐humped orbital modulations observed in SSS 0221−26, CSS 0345−01, CSS 1300+11 and CSS 1443−17 are typical of low‐mass transfer rate dwarf novae. The white dwarf primary of SDSS 0919+08 is confirmed to have non‐radial oscillations, and quasi‐periodic oscillations were observed in the short‐period dwarf nova CSS 1028−08 during outburst. We further report the detection of a new nova‐like variable (SDSS 1519+06). The frequency distribution of orbital periods of CVs in the Catalina Real‐time Transient Survey (CRTS) has a high peak near ∼80 min orbital period, independently confirming that found by Gänsicke et al. from SDSS sources. We also observe a marked correlation between the median in the orbital period distribution and the outburst class, in the sense that dwarf novae with a single observed outburst (over the 5‐year baseline of the CRTS coverage) occur predominantly at shortest orbital period.

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Section: Eg Aqr (Css 080101:232519−081819)mentioning

confidence: 98%

High-speed photometry of faint cataclysmic variables - VII. Targets selected from the Sloan Digital Sky Survey and the Catalina Real-time Transient Survey

Woudt

Warner

Budè

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…For example, stage-A was absent during the 2005 superoutburst of V391 Cam (Imada et al, 2009), despite the fact that the observations started from the onset of the superoutburst. Another example is the 2006 superoutburst of EG Aqr which showed a decrease of the superhump period during stage-B (Imada et al, 2008). Our statistical study suggests that systems with a superhump period longer than 0.08 days tend to show negative period derivatives during stage-B.…”

Section: Textbook Of Superhump Period Changementioning

confidence: 66%

Period Variations of Superhumps in Su Uma Stars

Imada¹,

Katô²

2015

Publications of The Korean Astronomical Society

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We review recent results on superhump period variations in SU UMa-type dwarf novae. Our statistical studies have revealed that the evolution of the superhump period is basically composed of three stages: stage-A, during which the superhump period is long and constant, stage-B, during which the superhump period increases as the superoutburst proceeds, and stage-C, during which the superhump period is short and constant. We also introduce a new method of estimating a mass ratio using the stage-A superhump period. This method can extend to, for example, low mass X-ray binaries or AM CVn stars if the stage-A superhump period is well determined.

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THEKEPLERLIGHT CURVES OF V1504 CYGNI AND V344 LYRAE: A STUDY OF THE OUTBURST PROPERTIES

Cannizzo

Smale

Wood

et al. 2012

ApJ

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We examine the Kepler light curves of V1504 Cyg and V344 Lyr, encompassing ∼736 d at 1 min cadence. During this span each system exhibited ∼64 − 65 outbursts, including six superoutbursts. We find that, in both systems, the normal outbursts lying between two superoutbursts increase in duration over time by a factor ∼1.2−1.9, and then reset to a small value after the following superoutburst. In both systems the trend of quiescent intervals between normal outbursts is to increase to a local maximum about half way through the supercycle − the interval from one superoutburst to the next − and then to decrease back to a small value by the time of the next superoutburst. This is inconsistent with Osaki's thermal-tidal model, which predicts a monotonic increase in the quiescent intervals between normal outbursts during a supercycle. Also, most of the normal outbursts have an asymmetric, fast-rise/slower-decline shape, which would be consistent with outbursts triggered at large radii. The exponential rate of decay of the plateau phase of the superoutbursts is 8 d mag −1 for V1504 Cyg and 12 d mag −1 for V344 Lyr. This time scale gives a direct measure of the viscous time scale in the outer accretion disk given the expectation that the entire disk is in the hot, viscous state during superoutburst. The resulting constraint on the Shakura-Sunyaev parameter, α hot 0.1, is consistent with the value inferred from the fast dwarf nova decays. By looking at the slow decay rate for superoutbursts, which occur in systems below the period gap, in combination with the slow decay rate in one long outburst above the period gap (in U Gem), we infer a steep dependence of the decay rate on orbital period for long outbursts. We argue that this relation implies a steep dependence of α cold on orbital period, which may be consistent with recent findings of Patterson, and is consistent with tidal torquing as being the dominant angular momentum transport mechanism in quiescent disks in interacting binary systems.

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The 2006 November Outburst of EG Aquarii: the SU UMa Nature Revealed

Cited by 8 publications

References 37 publications

High-speed photometry of faint cataclysmic variables - VII. Targets selected from the Sloan Digital Sky Survey and the Catalina Real-time Transient Survey

High-speed photometry of faint cataclysmic variables - VII. Targets selected from the Sloan Digital Sky Survey and the Catalina Real-time Transient Survey

Period Variations of Superhumps in Su Uma Stars

THEKEPLERLIGHT CURVES OF V1504 CYGNI AND V344 LYRAE: A STUDY OF THE OUTBURST PROPERTIES

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