Detection of superhumps in XTE J1118+480 approaching quiescence

Zurita, C.; Casares, J.; Shahbaz, T.; Wagner, R. M.; Foltz, C. B.; Rodríguez‐Gil, P.; Hynes, R. I.; Charles, P. A.; Ryan, Erin L.; Schwarz, G. J.; Starrfield, S.

doi:10.1046/j.1365-8711.2002.05450.x

Cited by 75 publications

(100 citation statements)

References 22 publications

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“…The orbital period is known to be 0.169937(1) days from the observed ellipsoidal modulation of the secondary in quiescence (Zurita et al 2002), and we adopt days as a mean value appropriate P p 0.17073 (12) sh to the eruption peak (within 0.4 mag of maximum light, the same convention we use in judging in dwarf novae). Thus P sh we obtain .…”

Section: ϫ6mentioning

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

232

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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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Section: ϫ6mentioning

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

232

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“…Two are the black hole X-ray binaries that display superhumps (Zurita et al 2002), the types of quasi-periodic oscillations (flickering) in dwarf novae (Warner & Woudt 2002), and the kinds of objects that display unidentified infrared features, the corona of Nova Cas 1995 having joined the cooler interstellar medium (Rudy et al 2002).…”

Section: Countdownmentioning

confidence: 99%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

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ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

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“…We may avoid the problem of the unknown pressure effect by using superhumps after the outburst. There is such an observation in KV UMa = XTE J1118+480 (Zurita et al 2002), reporting superhumps near quiescence having ε * = 0.0033.…”

Section: Late-stage Superhumps In Kv Ursae Majorismentioning

confidence: 97%

Survey of period variations of superhumps in SU UMa-type dwarf novae. V. The fifth year (2012–2013)

Katô¹,

Hambsch²,

Maehara³

et al. 2014

Publications of the Astronomical Society of Japan

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Continuing the project described in Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for SU UMa-type dwarf novae mainly observed during the 2012-2013 season. We found three objects (V444 Peg, CSS J203937, and MASTER J212624) having strongly positive period derivatives despite the long orbital period (P orb ). By using the period of growing stage (stage A) superhumps, we obtained mass ratios for six objects. We characterized nine new WZ Sge-type dwarf novae. We made a pilot survey of the decline rate in the slowly fading parts of SU UMa-type and WZ Sge-type outbursts. The decline time scale was found to generally follow an expected P 1/4 orb dependence, and WZ Sge-type outbursts also generally follow this trend. There are some objects which show slower decline rates, and we consider these objects good candidates for period bouncers. We also studied unusual behavior in some objects, including BK Lyn which made a transition from an ER UMa-type state to a novalike (standstill) state in 2013, and unusually frequent occurrences of superoutbursts in NY Ser and CR Boo. We applied the least absolute shrinkage and selection operator (Lasso) power spectral analysis, which has been proven to be very effective in analyzing the Kepler data, to the ground-based photometry of BK Lyn, and detected a dramatic disappearance of the signal of negative superhumps in 2013. We suggested that the mass-transfer rates did not strongly vary between the ER UMa-type state and novalike state in BK Lyn, and this transition was less likely caused by a systematic variation of the mass-transfer rate.

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Detection of superhumps in XTE J1118+480 approaching quiescence

Cited by 75 publications

References 22 publications

Astrophysics in 2002

Survey of period variations of superhumps in SU UMa-type dwarf novae. V. The fifth year (2012–2013)

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