1RXS J232953.9+062814: A Dwarf Nova with a 64 Minute Orbital Period and a Conspicuous Secondary Star

Thorstensen, J. R.; Fenton, William H.; Patterson, Joseph; Kemp, Jonathan; Krajci, Thomas; Baraffe, I.

doi:10.1086/339905

Cited by 111 publications

(130 citation statements)

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“…The hot donor star seen in the spectrum is the evolved core, stripped from its outer layers by the accretion process. Another such CV has recently been reported by Thorstensen (2013, CRTS J134052.1+151341) and it is thought that the same process is responsible for some sub-period minimum CVs, such as V485 Cen (Augusteijn, van Kerkwijk & van Paradijs 1993) and EI Psc (Thorstensen et al 2002). V544 Her is worthy of further observations.…”

Section: Donor Star Visible In the Continuummentioning

confidence: 62%

1000 cataclysmic variables from the Catalina Real-time Transient Survey

Breedt

Gänsicke

Drake

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Over six years of operation, the Catalina Real-time Transient Survey (CRTS) has identified 1043 cataclysmic variable (CV) candidates -the largest sample of CVs from a single survey to date. Here, we provide spectroscopic identification of 85 systems fainter than g ≥ 19, including three AM Canum Venaticorum binaries, one helium-enriched CV, one polar and one new eclipsing CV. We analyse the outburst properties of the full sample and show that it contains a large fraction of low-accretion-rate CVs with long outburst recurrence times. We argue that most of the high-accretion-rate dwarf novae in the survey footprint have already been found and that future CRTS discoveries will be mostly low-accretion-rate systems. We find that CVs with white-dwarf-dominated spectra have significantly fewer outbursts in their CRTS light curves compared to disc-dominated CVs, reflecting the difference in their accretion rates. Comparing the CRTS sample to other samples of CVs, we estimate the overall external completeness to be 23.6 per cent, but show that as much as 56 per cent of CVs have variability amplitudes that are too small to be selected using the transient selection criteria employed by current ground-based surveys. The full table of CRTS CVs, including their outburst and spectroscopic properties examined in this paper, is provided in the online materials.

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Section: Donor Star Visible In the Continuummentioning

confidence: 62%

1000 cataclysmic variables from the Catalina Real-time Transient Survey

Breedt

Gänsicke

Drake

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…11 are V485 Cen and EI Psc. While they have ultra-short orbital periods, their secondaries are relatively massive (Augusteijn et al 1993;Thorstensen et al 2002). The superhump period excess and mass ratio of EI Psc are ε = 0.040 and q = 0.19, respectively, which are actually larger than those of TV Crv and VW Hyi (Uemura et al 2002b).…”

Section: Discussionmentioning

confidence: 99%

TV Corvi revisited: Precursor and superhump period derivative linked to the disk instability model

Uemura

Mennickent²,

Ishioka

et al. 2005

A&A

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Abstract. We report optical photometric observations of four superoutbursts of the short-period dwarf nova TV Crv. This object experiences two types of superoutbursts; one with a precursor and the other without. The superhump period and period excess of TV Crv are accurately determined to be 0.065028 ± 0.000008 d and 0.0342 ± 0.0021, respectively. This large excess implies a relatively large mass ratio of the binary components (M 2 /M 1 ), though it has a short orbital period. The two types of superoutbursts can be explained by the thermal-tidal instability model for systems having large mass ratios. Our observations reveal that superhump period derivatives are variable in distinct superoutbursts. The variation is apparently related to the presence or absence of a precursor. We propose that the superhump period derivative depends on the maximum disk radius during outbursts. We investigate the relationship of the type of superoutbursts and the superhump period derivative for known sources. In the case of superoutbursts without a precursor, superhump period derivatives tend to be larger than those in precursor-main type superoutbursts, which is consistent with our scenario.

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“…All of these seem to be in binaries with hr P 1 8 orb (hence outside our net). And three others have radii that are much too small for their mass; these are all known or suspected to be helium rich (EI Psc: Thorstensen et al 2002a; QZ Ser: Thorstensen et al 2002b;and V485 Cen: Augusteijn et al 1996). But the great majority of CV secondaries seem to be pretty normal low-mass stars-just slightly agitated by the special circumstances of their imprisonment (enforced rapid rotation, struggles with thermal equilibrium, the occasional nova outburst, etc.…”

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confidence: 99%

Superhumps in Cataclysmic Binaries. XXV.q_crit, \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFont

Patterson

Kemp²,

Harvey

et al. 2005

PUBL ASTRON SOC PAC

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238

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ABSTRACT. We report on successes and failures in searching for positive superhumps in cataclysmic variables, and show the superhumping fraction as a function of orbital period. Basically, all short-period system do, all long-period systems do not, and a 50% success rate is found at hr. We can use this to measure P p 3.1 ‫ע‬ 0.2 orb the critical mass ratio for the creation of superhumps. With a mass-radius relation appropriate for cataclysmic variables, and an assumed mean white-dwarf mass of 0.75 M , , we find a mass ratio . We q p 0.35 ‫ע‬ 0.02 crit also report superhump studies of several stars of independently known mass ratio: OU Vir, XZ Eri, UU Aqr, and KV UMa (pXTE J1118ϩ480). The latter two are of special interest, because they represent the most extreme mass ratios for which accurate superhump measurements have been made. We use these to improve the (q) calibration, by which we can infer the elusive q from the easy-to-measure (the fractional period excess of over ). This relation allows mass and radius estimates for the secondary star in any cataclysmic P P superhump orb variable (CV) showing superhumps. The consequent mass-radius law shows an apparent discontinuity in radius near 0.2 M , , as predicted by the disrupted magnetic braking model for the 2.1-2.7 hr period gap. This is effectively the "empirical main sequence" for CV secondaries.

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1RXS J232953.9+062814: A Dwarf Nova with a 64 Minute Orbital Period and a Conspicuous Secondary Star

Cited by 111 publications

References 20 publications

1000 cataclysmic variables from the Catalina Real-time Transient Survey

1000 cataclysmic variables from the Catalina Real-time Transient Survey

TV Corvi revisited: Precursor and superhump period derivative linked to the disk instability model

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