A Search for Periodic and Quasi-periodic Photometric Behavior in the Cataclysmic Variable TT Arietis

Андронов, И. Л.; Arai, K.; Chinarova, L. L.; Dorokhov, N. I.; Dorokhova, T. N.; Dumitrescu, Alexandru; Nogami, Daisaku; Колесников, С. В.; Lepardo, A.; Mason, Paul; Matsumoto, Katsura; Oprescu, G.; Pajdosz, G.; Passuelo, R.; Patkos, L.; Senio, D. S.; Sostero, G.; Suleimanov, V.; Tremko, J.; Zhukov, G. V.; Zoła, S.

doi:10.1086/300665

Cited by 23 publications

(25 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Such quasiperiodic oscillations with a time-scale of 15-60 min are characteristic for some cataclysmic variables of similar orbital periods (e.g. Tremko et al 1996;Andronov et al 1999). However, our periodograms show no significant peaks at frequences, where the peaks have been found in previous years by Patterson & Thomas (1993) and Hellier (1999).…”

Section: Periodogram Analysissupporting

confidence: 47%

“…To make a set of quasi-simultaneous observations, the interpolating or smoothing technique is to be applied. For another cataclysmic variable TT Ari, we have used the method of "running parabolae" Andronov (1997) to make a set of simultaneous smoothed values in 3 colors UBV (Tremko et al 1996;Andronov et al 1999). That method is effective for stars with flickering-dominated variability.…”

Section: Quasi-simultaneous Vr Observationsmentioning

confidence: 99%

See 1 more Smart Citation

Orbital and spin variability of the intermediate polar BG CMi

Kim

Андронов

Park

et al. 2005

A&A

Self Cite

View full text Add to dashboard Cite

−25 E 4 . Thus the rate of the spin-up of the white dwarf is decreasing. An alternative explanation is that the spin-up has been stopped during recent years. The deviations between the amplitudes of the spin variability in V and R, as well as between phases are not statistically significant. However, the orbital light curves exhibit distinct difference; the corresponding color index shows a nearly sinusoidal shape with a maximum at orbital phase ∼0.2. The variations of the amplitude of spin waves shows a short maximum at the phase of the orbital dip. The corrected ephemeris for orbital minima is Min.HJD = 2 448 368.7225(12) + 0.d 13474841(6) · (E − 24849) with a narrow dip occuring 0.07P later. The rate of the spin period variation seems to be changed, justifying the necessity of regular observations of intermediate polars.

show abstract

Section: Periodogram Analysissupporting

confidence: 47%

Section: Quasi-simultaneous Vr Observationsmentioning

confidence: 99%

Orbital and spin variability of the intermediate polar BG CMi

Kim

Андронов

Park

et al. 2005

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…To study these different types of variability, several international observational campaigns were organized, the results of which were summarized by Wenzel et al (1986), Tremko et al (1996), Skillman et al (1998) and Andronov et al (1999). Hollander & van Paradijs (1992) proposed a dependence of QPO characteristics on accretion rate.…”

Section: Introductionmentioning

confidence: 99%

Nova-like cataclysmic variable TT Arietis

Kim

Андронов

et al. 2009

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We study the variability of the nova-like cataclysmic variable TT Ari, on time-scales of between minutes and months. Methods. The observations in the filter R were obtained at the 40-cm telescope of the Chungbuk National University (Korea), 51 observational runs cover 226 h. The table of individual observations is available electronically. In our analysis, we applied several methods: periodogram, wavelet, and scalegram analysis. Results. TT Ari remained in a "negative superhump" state after its return from the "positive superhump" state, which lasted for 8 years.The ephemeris for 12 of the best pronounced minima is T min = BJD 2 453 747.0700(47) + 0.132322(53)E. The phases of minima may reach 0.2, which reflects the non-eclipse nature of these minima. The quasi-periodic oscillations (QPO) are present with a mean "period" of 21.6 min and mean semi-amplitude of 36 mmag. This value is consistent with the range 15−25 min reported for previous "negative superhump" states and does not support the hypothesis of secular decrease in the QPO period. Either the period, or the semi-amplitude show significant night-to-night variations. According to the position at the two-parameter diagrams (i.e. diagrams of pairs of parameters: time, mean brightness of the system, brightness of the source of QPO, amplitude, and timescale of the QPOs), the interval of observations was divided into 5 parts, showing different characteristics: 1) the "pre-outburst" stage; 2) the "rise to outburst"; 3) "top of the outbursts"; 4) "post-outburst QPO" state; and 5) "slow brightening". The the QPO source was significantly brighter during the 10-day outburst, than during the preceding interval. However, after the outburst, the large brightness of the QPO source still existed for about 30 days, producing the stage "4". The diagram for m QPO (m) exhibits two groups in the brightness range 10. m 6−10. m 8, which correspond to larger and smaller amplitudes of the QPO. For the group "5" only, statistically significant correlations were found, for which, with increasing mean brightness, the period, amplitude, and brightness of the of QPO source also increase. The mean brightness at the "negative superhump state" varies within 10. m 3−11. m 2, so the system is brighter than at the "positive superhump" (11. m 3), therefore the "negative superhump" phenomenon may be interpreted by a larger accretion rate. The system is an excellent laboratory for studying processes resulting in variations on timescales of between seconds and decades and needs further monitoring at various states of activity.

show abstract

“…We have obtained almost 100 hours of observations for the cataclysmic variable TT Arietis (V = 9.5) in the multisite campaign organized by I. L. Andronov (Andronov et al 1999) in OctoberNovember 1994. One of 10 h runs per night is shown in Fig.…”

Section: Observations In Multisite Campaignsmentioning

confidence: 99%

Mt. Dushak-Erekdag Observatory: A Chance to Close the Asian Gaps in WET Coverage

Dorokhova

Dorokhov

2003

Open Astronomy

Self Cite

View full text Add to dashboard Cite

Abstract.The Mt. Dushak-Erekdag Observatory (Central Asia, Turkmenistan, 58 • E longitude) is located just in the longitudes gap of asteroseismological networks. It is the southernmost observatory of the former Soviet Union, its latitude is +38 • . The sky seeing at the site is one of the best in Central Asia: a low light pollution, high and stable sky transparency, over 200 usable nights per year. The altitude is above 2000 m.Odessa Astronomical Observatory has its 0.8 m telescope with a two-star high-speed photometer there, which frequently participates in international programs and multi-site campaigns. An accuracy of the photometry amounts to 1 mmag. Besides, a 1 m wide-angle telescope and a dual-tube telescope with 0.5 m mirrors are installed at the observatory.The developed infrastructure at the site and the stable economy in Turkmenistan make the Mt. Dushak-Erekdag Observatory very interesting for the WET observations.

show abstract

A Search for Periodic and Quasi-periodic Photometric Behavior in the Cataclysmic Variable TT Arietis

Cited by 23 publications

References 21 publications

Orbital and spin variability of the intermediate polar BG CMi

Orbital and spin variability of the intermediate polar BG CMi

Nova-like cataclysmic variable TT Arietis

Mt. Dushak-Erekdag Observatory: A Chance to Close the Asian Gaps in WET Coverage

Contact Info

Product

Resources

About