Superhump Evolution in the Ultrashort Period Dwarf Nova 1RXS J232953.9+062814

Uemura, Makoto; Katô, Takeo; Ishioka, Ryoko; Yamaoka, H.; Schmeer, P.; Krajci, Tom; Starkey, Donn R.; Torii, K.; Kawai, N.; Urata, Y.; Kohama, M.; Yoshida, A.; Ayani, K.; Kawabata, Tetsuya; Tanabe, Kenji; Matsumoto, Katsura; Kiyota, S.; Pietz, J.; Vanmunster, Tonny; Oksanen, A.; Giambersio, Antonio

doi:10.1093/pasj/54.4.599

Cited by 30 publications

(22 citation statements)

References 24 publications

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“…The argument for a very low mass, late-type donor (Section 3.4) is further supported by the mass ratios of those binaries, which are less extreme than that of CSS1122−1110. For V485 Cen, we use the P sh measurement of Olech (1997) to calculate q = 0.13 ± 0.01, and for EI Psc, the P sh estimate from Uemura et al (2002) gives q = 0.14 ± 0.01. The mass ratio we find for CSS1122−1110 is much more extreme, q = 0.017 ± 0.004.…”

Section: Figurementioning

confidence: 99%

CSS100603:112253−111037: a helium-rich dwarf nova with a 65 min orbital period

Breedt

Gänsicke

Marsh

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present time‐resolved optical spectroscopy of the dwarf nova CSS100603:112253−111037. Its optical spectrum is rich in helium, with broad, double‐peaked emission lines produced in an accretion disc. We measure a line flux ratio He i λ5876/Hα = 1.49 ± 0.04, a much higher ratio than is typically observed in dwarf novae. The orbital period, as derived from the radial velocity of the line wings, is 65.233 ± 0.015 min. In combination with the previously measured superhump period, this implies an extreme mass ratio of M2/M1 = 0.017 ± 0.004. The Hα and He i λ 6678 emission lines additionally have a narrow central spike, as is often seen in the spectra of AM CVn‐type stars. Comparing their properties with cataclysmic variables (CVs), AM CVn systems and hydrogen binaries below the CV period minimum, we argue that CSS100603:112253−111037 is the first compelling example of an AM CVn system forming via the evolved CV channel. With the addition of this system, evolved CVs now account for 7 per cent of all known semidetached white dwarf binaries with Porb < 76 min. Two recently discovered binaries may further increase this figure. Although the selection bias of this sample is not yet well defined, these systems support the evolved CV model as a possible formation channel for ultracompact accreting binaries. The orbital periods of the three ultracompact hydrogen accreting binaries overlap with those of the long‐period AM CVn stars, but there are currently no known systems in the period range of 67–76 min.

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Section: Figurementioning

confidence: 99%

CSS100603:112253−111037: a helium-rich dwarf nova with a 65 min orbital period

Breedt

Gänsicke

Marsh

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…In order to thoroughly investigate the short period system, the VSNET ) has placed V844 Her as one of the highest priorities since the confirmation of the SU UMa nature of the system. In 2002May, 2002October, and 2003 October, V844 Her underwent an outburst and the VSNET Collaboration Team detected superhumps during these superoutbursts.…”

Section: Introductionmentioning

confidence: 99%

Long-Term Monitoring of the Short Period SU UMa-Type Dwarf Nova, V844 Herculis

Oizumi

Omodaká

Yamamoto

et al. 2007

Publications of the Astronomical Society of Japan

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We report on time-resolved CCD photometry of four outbursts of a short-period SU UMa-type dwarf nova, V844 Herculis. We successfully determined the mean superhump periods to be 0.05584(64) days, and 0.055883(3) for the 2002 May superoutburst, and the 2006 April-May superoutburst, respectively. During the 2002 October observations, we confirmed that the outburst is a normal outburst, which is the first recorded normal outburst in V844 Her. We also examined superhump period changes during 2002 May and 2006 April-May superoutbursts, both of which showed increasing superhump period over the course of the plateau stage. In order to examine the long-term behavior of V844 Her, we analyzed archival data over the past ten years since the discovery of this binary. Although photometry is not satisfactory in some superoutbursts, we found that V844 Her showed no precursors and rebrightenings. Based on the long-term light curve, we further confirmed V844 Her has shown almost no normal outbursts despite the fact that the supercycle of the system is estimated to be about 300 days. In order to explain the long-term light curves of V844 Her, evaporation in the accretion disk may play a role in the avoidance of several normal outbursts, which does not contradict with the relatively large X-ray luminosity of V844 Her.

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“…The open circles are fromKato et al (2001b). The data points of 1RXS J232953.9+062814 and V725 Aql are fromUemura et al (2002b) andUemura et al (2001).…”

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confidence: 99%

Photometric study of new southern SU UMa-type dwarf novae and candidates: V877 Ara, KK Tel and PU CMa

Katô

Santallo

Bolt³

et al. 2003

Monthly Notices of the Royal Astronomical Society

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We photometrically observed the three dwarf novae V877 Ara, KK Tel and PU CMa. We discovered the undisputed presence of superhumps in V877 Ara and KK Tel, with mean periods of 0.084 11(2) and 0.088 08(3) d, respectively. Both V877 Ara and KK Tel are confirmed to belong to long‐period SU UMa‐type dwarf novae. In V877 Ara, we found a large decrease of the superhump period . There is evidence that the period of KK Tel decreased at a similar or a more exceptional rate. Coupled with the past studies of superhump period changes, these findings suggest that a previously neglected diversity of phenomena is present in long‐period SU UMa‐type dwarf novae. The present discovery of a diversity in long‐period SU UMa‐type systems would become an additional step towards a full understanding of the dwarf nova phenomenon. PU CMa is shown to be an excellent candidate for an SU UMa‐type dwarf nova. We examined the outburst properties of these dwarf novae, and derived characteristic outburst recurrence times. Combined with the recently published measurement of the orbital period of PU CMa, we propose that PU CMa is the first object filling the gap between the extreme WZ Sge‐type and ER UMa‐type stars.

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Superhump Evolution in the Ultrashort Period Dwarf Nova 1RXS J232953.9+062814

Cited by 30 publications

References 24 publications

CSS100603:112253−111037: a helium-rich dwarf nova with a 65 min orbital period

CSS100603:112253−111037: a helium-rich dwarf nova with a 65 min orbital period

Long-Term Monitoring of the Short Period SU UMa-Type Dwarf Nova, V844 Herculis

Photometric study of new southern SU UMa-type dwarf novae and candidates: V877 Ara, KK Tel and PU CMa

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