Detection of superhumps and quasi-periodic oscillations in the light curve of the dwarf nova SW Ursae Majoris

1987 ◽  
Vol 313 ◽  
pp. 772 ◽  
Author(s):  
Edward L. Robinson ◽  
Allen W. Shafter ◽  
J. Allen Hill ◽  
Matt A. Wood ◽  
Janet A. Mattei
Keyword(s):  
Light Curve ◽  
Periodic Oscillations ◽  
Dwarf Nova

scholarly journals Quasi-Periodic and Periodic Oscillations in the Dwarf Nova AH Her

1979 ◽  
Vol 53 ◽  
pp. 403-403
Author(s):  
J.G. Duthie ◽  
R.S. McMillan
Keyword(s):  
Light Curve ◽  
Autocorrelation Function ◽  
High Speed ◽  
Statistical Significance ◽  
Cataclysmic Variables ◽  
Power Spectra ◽  
Photometric System ◽  
Periodic Oscillations ◽  
Dwarf Nova ◽  
High Statistical Significance

With a high speed photometric system we have made extensive observation of the dwarf nova AH Her. We have detected rapid oscillations on two consecutive nights during the recovery portion of the light curve of a typical outburst during the spring of 1979. The periods and the sense of the change of period are consistent with previous observations of rapid oscillations of AH Her. On another occasion we detected quasi-periodic oscillations during the rising portion of an outburst. These are similar in appearance to quasi-periodic oscillations found in other cataclysmic variables in that they appear with high statistical significance in the autocorrelation function but are not apparent in power spectra (Robinson and Nather 1979). However they are different from those reported by Robinson and Nather in the sense that they have the same order of period as the periodic rapid oscillations typical of AH Her. These results will be presented together with a discussion of their Implications.

Simultaneous infrared and optical photometry of the Eclipsing Dwarf Nova V2051 Ophiuchi

1986 ◽  
Vol 6 (3) ◽  
pp. 306-308 ◽  
Author(s):  
D. J. Watts ◽  
R. D. Watson
Keyword(s):  
Light Curve ◽  
Optical Photometry ◽  
Dwarf Nova

AbstractA complete orbital light-curve of V2051 Oph in the IR H band is presented, together with a second eclipse in the J band. Simultaneous Rc band data were obtained. Eclipse depths in Rc, J and H are 1.8 mag, 1.0 mag and 0.8 mag respectively. No evidence for ellipsoidal variations due to the secondary was seen and constraints on the secondary are discussed.

On the Spectrum of VV Puppis

1979 ◽  
Vol 3 (5) ◽  
pp. 311-312 ◽  
Author(s):  
D. T. Wickramasinghe ◽  
N. Visvanathan
Keyword(s):  
Light Curve ◽  
Hot Spot ◽  
Accretion Disc ◽  
Dwarf Nova ◽  
Spot Model ◽  
Hot Spot Model ◽  
Linear Polarisation

Since the discovery of variable circular and linear polarisation in VV Puppis (Tapia 1977), several investigators have observed the system. The new observations particularly of polarisation (Liebert et al. 1978, Liebert and Stockman 1979 have ruled out the standard dwarf nova (accretion disc — hot spot) model previously used to interpret the light curve of VV Puppis.

scholarly journals Probing the X-ray Variability of X-ray Binaries

2003 ◽  
Vol 214 ◽  
pp. 236-239
Author(s):  
Wenfei Yu
Keyword(s):  
Neutron Star ◽  
Light Curve ◽  
Time Scale ◽  
Accretion Rate ◽  
Power Spectra ◽  
The Other ◽  
Periodic Oscillations ◽  
X Ray ◽  
Orbital Frequency ◽  
X Ray Binaries

Kilohertz quasi-periodic oscillations (kHz QPOs) has been regarded as representing the Keplerian frequency at the inner disk edge in the neutron star X-ray binaries. The so-called “parallel tracks” on the plot of the kHz QPO frequency vs. X-ray flux in neutron star X-ray binaries, on the other hand, show the correlation between the kHz QPO frequency and the X-ray flux on time scales from hours to days. This is suspected as caused by the variations of the mass accretion rate through the accretion disk surrounding the neutron star. We show here that by comparing the correlation between the kHz QPO frequency and the X-ray count rate on a certain QPO time scale observed approximately simultaneous in the Fourier power spectra of the X-ray light curve, we have found evidences that the X-ray flux of millihertz QPOs in neutron star X-ray binaries is generated inside the inner disk edge if adopting that the kilohertz QPO frequency is an orbital frequency at the inner disk edge.

scholarly journals Mapping Quasi-Periodic Oscillations from the Outbursting Intermediate Polar GK Persei

1997 ◽  
Vol 163 ◽  
pp. 809-810
Author(s):  
M. D. Still ◽  
L. Morales-Rueda ◽  
P. Roche
Keyword(s):  
Optical Emission ◽  
Accretion Disc ◽  
Emission Lines ◽  
Periodic Oscillations ◽  
Dwarf Nova ◽  
Nova Outburst

AbstractWe provide a kinematically-resolved analysis of 5000s QPOs found in the optical emission lines of GK Per during a dwarf nova outburst. These are consistent with models of reprocessing off blobs of gas orbiting within the inner accretion disc.

scholarly journals Dwarf Nova Oscillations and Quasi-Periodic Oscillations: Extension of the Two-QPO Diagram of X-Ray Binaries, and a new kind of DNO

2004 ◽  
Vol 190 ◽  
pp. 85-90
Author(s):  
Brian Warner ◽  
Patrick A. Woudt
Keyword(s):  
White Dwarf ◽  
Cataclysmic Variable ◽  
Periodic Oscillations ◽  
X Ray ◽  
Dwarf Nova ◽  
X Ray Binaries

AbstractSeventeen examples are given of Cataclysmic Variable (CV) stars possessing both Dwarf Nova Oscillations (DNOs) and Quasi-Periodic Oscillations (QPOs). These form an extension of the X-Ray Two-QPO correlation to frequencies three orders of magnitude lower. We draw attention to the existence of a second type of DNO in CVs, which is probably caused by magnetically channelled accretion onto the white dwarf.

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