Variability of the spin period of the white dwarf in the intermediate polar v405 aur:  low-mass third body or precession?

Breus, V. V.; Андронов, И. Л.; Dubovský, Pavol A.; Колесников, С. В.; Zhuzhulina, E. A.; Hegedüs, T.; Beringer, P.; Petrik, K.; Robertson, J. W.; Ryabov, Andrey V.; Kudzej, Igor; Shakhovskoy, N. M.

doi:10.30970/jps.17.3901

Cited by 7 publications

(6 citation statements)

References 16 publications

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“…Sometimes, semi-regular variables show two very different periods. This phenomenologically resembles intermediate polars, in which the two very distinct periods are seen, although they have different nature (Breus et al, 2012;Breus et al, 2013).…”

Section: Periodogram Analysis Of Rv Tau-type Starsmentioning

confidence: 85%

“…The Group III includes objects, the periodograms of which are highly noisy, mainly due to a small number of observations or they do not show typical structures of RV-type stars (figures 1-3).Sometimes, semi-regular variables show two very different periods. This phenomenologically resembles intermediate polars, in which the two very distinct periods are seen, although they have different nature(Breus et al, 2012;Breus et al, 2013).The mean light curves with the statistically best period, the approximations are computed using the program MCV(Andronov and Baklanov, 2004;. These light curves are shown in the figure4.…”

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confidence: 95%

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Multi-Component Variability of Pulsating Variable Stars of Rv Tauri Type

Kudashkina

2020

OAP

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For the group of pulsating variable stars with multi-component variabilitywhich are currently classified as the RV Tau-type starsthe classification based on complexity of the periodograms is discussed. Periodograms were computed using the least approximation of the data with a sinusoid. The periodograms previously classified by their shape into three groups according to the presence or absence of certain structures: two peaks in a 2:1 ratio, (biharmonic signal with two waves during a main period, or the phase curve is significantly asymmetric), the presence of satellites of these peaks at the periodogram indicating the result of modulation of characteristics of oscillations. Group I includes objects showing the periodogram typical for the RV-type stars, and the ratio of the periods of the two main peaks is indicated. These oscillations appear to be relatively stable during the observations. The Group II includes objects, the periodograms of which contain signs of multi-periodicity or, vice-versa, only one clear peak, instead of two. The presence of multiple peaks may be due to multiple periods, or due to variability of the main period. The Group III includes objects, the periodograms of which are highly noisy, mainly due to a small number of observations or they do not show typical structures of RVtype stars. Such stars may be classified in the catalogue wrongly, so, additional study is needed. For periodogram analysis, the photometric observations from the international databases of AFOEV, AAVSO and ASAS were used. A least squares method is used for the analysis, to compare the variance in the deviations from the smoothed function with the variance in the initial observations. The mean light curves and the phase plane diagrams dxC()/d vs xC() was compiled and analyzed for the values of the periods corresponding to the peaks in the periodograms.

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Section: Periodogram Analysis Of Rv Tau-type Starsmentioning

confidence: 85%

mentioning

confidence: 95%

Multi-Component Variability of Pulsating Variable Stars of Rv Tauri Type

Kudashkina

2020

OAP

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“…Other intermediate polars show for decades either an increase of the period, or its subsequent decrease (e.g. FO Aqr [31], V405 Aur [32]).…”

Section: Discussionmentioning

confidence: 99%

Variability of the Rotation Period of the White Dwarf in the Magnetic Cataclysmic Binary System EX Hya

Андронов

Breus²

2013

Astrophysics

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The observations of the two-periodic magnetic cataclysmic system EX Hya have been carried out, using the telescopes RC16 and TOA-150 of the Tzec Maun observatory. 6 nights of observations were obtained in 2010-2011 (alternatively changing filters VR). Also the databases of WASP, ASAS and AAVSO have been analyzed. Processing time series was carried out using the program MCV. We analyzed changes in the rotation period of the white dwarf, and based on our own and previously published moments of maximum. The ephemeris was determined for the maxima of the radiation flux associated with the rotation of the magnetic white dwarf:

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“…Some objects do not show a statistically significant period change (e.g.1RXS J180340.0 + 401214 = RXJ 1803 = V1323 Her [13], some show a period decrease (e.g. BG CMi [14], EX Hya [15], [16]), some show a period increase, but some show increase and decrease during a couple decades of observations (e.g. FO Aqr [17]).…”

Section: Discussionmentioning

confidence: 99%

Variability of the Spin Period of the White Dwarf in the Intermediate Polar V405 Aur: Low-Mass Third Body or Precession ?

Breus¹,

Андронов²,

Dubovský³

et al. 2013

Preprint

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We present the results of photometric CCD observations of the magnetic cataclysmic variable V405 Aurigae (RX J0558.0+5353 = 1RXS J055800.7+535358) obtained using different instruments. We analysed variability of the spin period of the white dwarf in the V405 Aur (RX J0558.0+5353) system using our observations and previously published maxima timings. The spin period of the system in 2010-2012 is P = 545.4558163(94)s. As we have gaps in observational data, we present 2 hypotheses of the spin period variability of this system -a cubic ephemeris which may be interpreted by a precession of the magnetic white dwarf or a periodic change with a period of 6.2 years and semi-amplitude of 17.2 ± 1.8 sec. The periodic variations may be interpreted by a lighttime effect caused by a low-mass star (M 3 ≥ 0.09M ). In this case, the system belongs to a rare class of cataclysmic variables with a third body.

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Variability of the spin period of the white dwarf in the intermediate polar v405 aur: low-mass third body or precession?

Cited by 7 publications

References 16 publications

Multi-Component Variability of Pulsating Variable Stars of Rv Tauri Type

Multi-Component Variability of Pulsating Variable Stars of Rv Tauri Type

Variability of the Rotation Period of the White Dwarf in the Magnetic Cataclysmic Binary System EX Hya

Variability of the Spin Period of the White Dwarf in the Intermediate Polar V405 Aur: Low-Mass Third Body or Precession ?

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