The Orbital Period and Variability of the Dwarf Nova WW Ceti

1996 ◽  
Vol 111 ◽  
pp. 2077 ◽  
Author(s):  
F. A. Ringwald ◽  
John R. Thorstensen ◽  
R. Kent Honeycutt ◽  
Robert Connon Smith
Keyword(s):  
Orbital Period ◽  
Dwarf Nova

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

2002 ◽  
Vol 567 (1) ◽  
pp. L49-L52 ◽  
Author(s):  
John R. Thorstensen ◽  
William H. Fenton ◽  
Joseph O. Patterson ◽  
Jonathan Kemp ◽  
Thomas Krajci ◽  
...  
Keyword(s):  
Orbital Period ◽  
Dwarf Nova ◽  
Secondary Star

scholarly journals Superoutbursts and Superhumps of SU UMa Stars

1988 ◽  
Vol 108 ◽  
pp. 238-239
Author(s):  
Yoji Osaki ◽  
Masahito Hirose
Keyword(s):  
Accretion Disk ◽  
Orbital Period ◽  
White Dwarf ◽  
Binary Systems ◽  
Roche Lobe ◽  
Light Curves ◽  
Close Binary ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Close Binary Systems

SU UMa stars are one of subclasses of dwarf novae. Dwarf novae are semi-detached close binary systems in which a Roche-lobe filling red dwarf secondary loses matter and the white dwarf primary accretes it through the accretion disk. The main characteristics of SU UMa subclass is that they show two kinds of outbursts: normal outbursts and superoutbursts. In addition to the more frequent narrow outbursts of normal dwarf nova, SU UMa stars exhibit “superoutbursts”, in which stars reach about 1 magnitude brighter and stay longer than in normal outburst. Careful photometric studies during superoutburst have almost always revealed the “superhumps”: periodic humps in light curves with a period very close to the orbital period of the system. However, the most curious of all is that this superhump period is not exactly equal to the orbital period, but it is always longer by a few percent than the orbital period.

scholarly journals A Beat Phenomenon in Dwarf Nova Eruptions

1977 ◽  
Vol 42 ◽  
pp. 227-233
Author(s):  
N. Vogt
Keyword(s):  
Mass Transfer ◽  
Orbital Period ◽  
Transfer Rate ◽  
Convection Zone ◽  
Mass Transfer Rate ◽  
Accretion Disc ◽  
Light Curves ◽  
Dwarf Nova ◽  
Beat Phenomenon ◽  
Photoelectric Observations

Photoelectric observations of the dwarf nova VW Hyi, obtained at the end of the December 1975 supermaximum, are presented. After decline from the outburst, the superhump period (0ḍ07622) combines with the orbital period (0ḍ07427) to a beat phenomenon: the O-C’s and the light curves of the orbital hump vary systematically with the phase of the beat period for at least one week after recovery from the supermaximum. It is suggested that the red secondary component, which rotates non-synchroneously with the superhump period, expands slightly at the beginning of a supermaximum and is heated up asymmetrically, probably due to instabilities in its convection zone. In addition, the increased mass transfer rate may trigger the long eruption in the accretion disc while short eruptions originate in the disc without participation of the secondary.

scholarly journals Dwarf Novae in the Shortest Orbital Period Regime. I A New Short Superhump Period Dwarf Nova, OT J055717+683226

2010 ◽  
Vol 62 (1) ◽  
pp. 187-199 ◽  
Author(s):  
Makoto Uemura ◽  
Akira Arai ◽  
Taichi Kato ◽  
Hiroyuki Maehara ◽  
Daisaku Nogami ◽  
...  
Keyword(s):  
Orbital Period ◽  
Dwarf Novae ◽  
Dwarf Nova

scholarly journals Characterising the Dwarf Nova Population of the Catalina Real-time Transient Survey

2011 ◽  
Vol 7 (S285) ◽  
pp. 301-302
Author(s):  
Deanne de Budè ◽  
Patrick Woudt ◽  
Brian Warner
Keyword(s):  
Real Time ◽  
Orbital Period ◽  
High Speed ◽  
Photometric Study ◽  
Dwarf Novae ◽  
Dwarf Nova

AbstractResults of a high-speed photometric study of dwarf novæ in the Catalina Real-time Transient Survey are given. A population of faint dwarf novæ near the orbital period minimum is detected. At the shortest periods there is a correlation between orbital period and outburst interval.

scholarly journals Dwarf Nova-Like Outburst of Short-Period Intermediate Polar HT Camelopardalis

2004 ◽  
Vol 194 ◽  
pp. 259-259
Author(s):  
R. Ishioka ◽  
Keyword(s):  
Orbital Period ◽  
Alternative Interpretation ◽  
Cataclysmic Variable ◽  
Optical Counterpart ◽  
X Ray ◽  
Dwarf Nova ◽  
Spin Period ◽  
Photometric Observations ◽  
Sky Survey ◽  
Short Period

Our time-series photometric observations of a short outburst of HT Cam in 2001 strongly suggest that disk instabilities occurred during the outburst.HT Cam is a cataclysmic variable identified as the optical counterpart of the hard X-ray source RX J0757.0+6306, discovered during the ROSAT All-Sky Survey. Tovmassian et al. (1998) suggested that this object is an intermediate polar with a shortest orbital period of 80.92min and a spin period of 8.52min. However, the existence of dwarf nova-like outbursts and the short orbital period allowed an alternative interpretation that it may be an SU UMa-type dwarf nova or WZ Sge-type stars (Tovmassian et al. 1998).

scholarly journals QZ Serpentis: A Dwarf Nova with a 2 Hour Orbital Period and an Anomalously Hot, Bright Secondary Star

2002 ◽  
Vol 114 (800) ◽  
pp. 1117-1123 ◽  
Author(s):  
John R. Thorstensen ◽  
William H. Fenton ◽  
Joseph Patterson ◽  
Jonathan Kemp ◽  
Jules Halpern ◽  
...  
Keyword(s):  
Orbital Period ◽  
Dwarf Nova ◽  
Secondary Star

scholarly journals Superoutburst of a New Sub-Period-Minimum Dwarf Nova CSS130418 in Hercules

2015 ◽  
Vol 2 (1) ◽  
pp. 165-169 ◽  
Author(s):  
D. Chochol ◽  
S. Shugarov ◽  
N. Katysheva ◽  
I. Volkov ◽  
A. Zharova ◽  
...  
Keyword(s):  
Accretion Disk ◽  
Stellar Evolution ◽  
Orbital Period ◽  
Late Stage ◽  
Cataclysmic Variables ◽  
Light Curves ◽  
Dwarf Nova ◽  
The Mean ◽  
Normal Hydrogen

Multicolour photometry of a new dwarf nova CSS130418 in Hercules, which underwent superoutburst on April 18, 2013, allow to classified it as a WZ Sge-type dwarf nova. The phase light curves for different stages of superoutburst are presented. The early superhumps were used to determine the orbital period P<sub>orb</sub> = 64.84(1) minutes, which is shorter than the period minimum ~78 minutes for normal hydrogen-rich cataclysmic variables. We found the mean period of ordinary superhumps P<sub>sh</sub> = 65.559(1) minutes. The quiescent spectrum is rich in helium, showing double peaked emission<br />lines of H I and He I from accretion disk, so the dwarf nova is in a late stage of stellar evolution.

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