Long-Term Brightness Changes of Two CVS

Sokolov, D. A.; Shugarov, S. Yu.; Павленко, Е. П.

doi:10.1007/978-94-009-0325-8_65

Cited by 3 publications

(1 citation statement)

References 2 publications

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“…The first one was recorded on photographs taken in 1969 (Sokolov et al 1996), a second one in 1999 (Watanabe 1999;Kato & Uemura 1999), and recently a third one, albeit poorly sampled . Judging by the general pattern and the time-scale of the recovery from minimum, Kato & Uemura (1999) placed LQ Peg among the VY Scl subgroup of NL CVs.…”

Section: Lq Pegmentioning

confidence: 99%

Photometric study of selected cataclysmic variables

Papadaki

Boffin

Sterken

et al. 2006

A&A

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Aims. We present time-resolved photometry of five relatively poorly-studied cataclysmic variables: V1193 Ori, LQ Peg, LD 317, V795 Her, and MCT 2347-3144. Methods. The observations were made using four 1m-class telescopes for a total of more than 250 h of observation and almost 16 000 data points. For LQ Peg WHT spectroscopic data have been analysed as well. Results. The light curves show a wide range of variability on different time scales from minutes to months. We detect for the first time a brightness variation of 0.05 mag in amplitude in V1193 Ori on the same timescale as the orbital period, which we interpret as the result of the irradiation of the secondary. A 20-min quasi-periodic oscillation is also detected. The mean brightness of the system has changed by 0.5 mag on a three-month interval, while the flickering was halved. In LQ Peg a 0.05 mag modulation was revealed with a period of about 3 h. The flickering was much smaller, of the order of 0.025 mag. A possible quasi-periodic oscillation could exist near 30 min. For this object, the WHT spectra are single-peaked and do not show any radial-velocity variations. The data of LD 317 show a decrease in the mean magnitude of the system. No periodic signal was detected but this is certainly attributable to the very large flickering observed: between 0.07 and 0.1 mag. For V795 Her, the 2.8-h modulation, thought to be a superhump arising from the precession of the disc, is present. We show that this modulation is not stable in terms of periodicity, amplitude, and phase. Finally, for MCT 2347-3144, a clear modulation is seen in a first dataset obtained in October 2002. This modulation is absent in August 2003, when the system was brighter and showed much more flickering.

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Section: Lq Pegmentioning

confidence: 99%

Photometric study of selected cataclysmic variables

Papadaki

Boffin

Sterken

et al. 2006

A&A

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QPOS of By Cam in Low and High States

Павленко¹,

Shugarov²,

Antipin³

et al. 1996

International Astronomical Union Colloquium

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Abstract. We present the analysis of BV photometry of BY Cam based on observations carried out in Crimea. The long QPOs in brightness were detected in both high and low brightness states. Their typical periods, equal to 6, 12 and 24 m, are found. The amplitude of the QPOs depends on the phase of Pbeat- ResultsBY Cam is an AM Her type binary discovered by Remillard et al. (1986). It is the second, after the polar V1500 Cyg, to show asynchronism of the white dwarf's spin with respect to the binary and a fast synchronization of the components (Mason et al. 1995). BY Cam shows very complicated behaviour in optical light due to the existence of several periods: orbital, orbital side-band, spin and spin-orbit beat periods (Mason et al. 1995).The observations of BY Cam were carried out at the Crimean Astrophysical Observatory and Sternberg Astronomical Institute with the 0.5, 0.6 and 1.25 m telescopes using the BVR system during 25 nights from 1989 up to 1994. The long-term BVR light curve is shown by Sokolov, Shugarov & Pavlenko (1996).One of the most intriguing and unresolved problems in studying BY Cam is the evidence of the so-called long (tens of minutes) quasi-periodic brightness oscillations. They appear both in a low and high brightness state and have a varying amplitude, which sometimes increases up to 0.3 mag.Adopting Pbeat = 14.11 d and P s p i n = 0.1384238d (Mason et al. 1995), we have analysed the behaviour of the QPOs amplitude with the phase of Pbe&t (or with O -C of P sp j n for both minima and maxima). The elements: 217A. Evans and J. H. Wood (eds.), Cataclysmic Variables and Related Objects,[217][218]

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Characteristics of High-State/Low-State Transitions in VY Sculptoris Stars

Honeycutt

Kafka

2004

Astron J

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Long-Term Brightness Changes of Two CVS

Cited by 3 publications

References 2 publications

Photometric study of selected cataclysmic variables

Photometric study of selected cataclysmic variables

QPOS of By Cam in Low and High States

Characteristics of High-State/Low-State Transitions in VY Sculptoris Stars

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