Two-Color Vr CCD Photometry of the Intermediate Polar `Rxs J062518.2+733433

Kim, Yong-Gi; Андронов, И. Л.; Park, Sungsu; Chinarova, L. L.; Baklanov, Alexey V.; Jeon, Young‐Beom

doi:10.5140/jass.2005.22.3.197

Cited by 18 publications

(25 citation statements)

References 6 publications

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“…Staude et al (2003) reported a relativly strong HeII emission line which shows the existence of photons able to ionize the atoms. This characteristic has been discussed by other authors (Araujo-Betancor et al 2003, Staude et al 2003, 2008, Kim et al 2005a, Kozhevnikov et al 2006. These observational characteristics led to the classification of this object as an intermediate polar or DQ Her type magnetic cataclysmic variable.…”

Section: Introductionsupporting

confidence: 64%

“…The found spin period of MU Cam, 0. d 01373801(59), seems to be the same value as Staude et al (2003) and Kim et al (2005a) in the error interval. But it is necessary to check for the possible period variations, P  , which are usually seen in intermediate polars.…”

Section: Resultsmentioning

confidence: 90%

“…1. A bright state and a faint state are not shown in this season, which is clearly seen by Kim et al (2005a).…”

Section: Observation and Analysismentioning

confidence: 81%

“…In the method of multiple comparison stars, an independent R brightness estimate of 7 bright stars in the vicinity of the MU Cam was made based on the method described in Kim et al (2005a). The standardized R light curve has been obtained by using an artificial star which made it possible to increase accuracy estimates.…”

Section: Observation and Analysismentioning

confidence: 99%

“…Many corrections of the MU Cam spin period have been reported by several authors (Araujo- Betancor et al 2003, Staude et al 2003, Kim et al 2005a. In order to study the rotational evolution of magnetic white dwarfs in intermediate polars, a long time-base monitoring of the spin period variation is definitely needed.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Long-Term Variation of the Spin Period of a Magnetic Cataclysmic Variable, MU Camelopardalis

Yun¹,

Kim²,

Choi³

2011

Journal of Astronomy and Space Sciences

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Section: Introductionsupporting

confidence: 64%

Section: Resultsmentioning

confidence: 90%

“…1. A bright state and a faint state are not shown in this season, which is clearly seen by Kim et al (2005a).…”

Section: Observation and Analysismentioning

confidence: 81%

Section: Observation and Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Long-Term Variation of the Spin Period of a Magnetic Cataclysmic Variable, MU Camelopardalis

Yun¹,

Kim²,

Choi³

2011

Journal of Astronomy and Space Sciences

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The new period of the intermediate polar V709 Cas

et al. 2014

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We present the results of 10 years of photometric CCD observations of the intermediate polar V709 Cas obtained by using different instruments during 2003–2013. We detected a new variability with a period of Pnew = 0.d016449979(5) which seems to be real. The spin variability is not clearly seen in all our data, so we are unable to study any evolution of the white dwarf rotation. From the best night (in 2010) we obtained a spin period of Pspin = 311.s8(5). We analyzed the orbital variability using (O – C) analysis. We found no variations of the orbital period on a timescale of 10 years, but the linear fit to the (O – C) diagram shows that the value of the orbital period is Porb = 0.d2222123(6), which is close to the earlier published values. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Extensive photometry of the intermediate polar MU Cam: detection of a spin period change

Kozhevnikov

2016

Astrophys Space Sci

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Intermediate polars with known rates of spin period changes are not numerous because such tasks require measurements performed for a long time.To measure a spin period change, MU Cam is a good candidate because it has a spin oscillation with a large amplitude enabling measurements with high precision. Fortunately, in the past the spin period of MU Cam was measured with high precision. To measure the spin period anew, in 2014-2015 we performed extensive photometric observations of MU Cam, spanning a total duration of 208 h within 46 nights. We found that the spin, sideband and orbital periods are equal to 1187.16245 ± 0.00047 s, 1276.3424 ± 0.0022 s and 4.71942 ± 0.00016 h, respectively. Comparing the measured spin period with the spin period of MU Cam in the past, we detected the spin period change with dP/dt = −(2.17 ± 0.10) × 10 −10 . This rate of the spin period change was not stable and varied in a time scale of years. During four nights in 2014 April-May MU Cam was fainter than usual by 0.8 mag, and the amplitude of the sideband oscillation was five times larger, denoting significant fraction of disc-overflow accretion. The sideband oscillation showed a doublepeaked pulse profile in the normal brightness state. When the star brightness was decreased by 0.8 mag, the sideband oscillation showed a single-peaked pulse profile. In contrast, the spin pulse, which was quasisinusoidal, remained remarkably stable both in profile and in amplitude. Moreover, the spin pulse was also remarkably stable in a time scale of years and even decades. MU Cam is of great interest because it represents a distinctive object with a large and unstable rate of the spin period change and exhibits a distinctive behaviour of the pulse profiles.

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Two-Color Vr CCD Photometry of the Intermediate Polar `Rxs J062518.2+733433

Cited by 18 publications

References 6 publications

Long-Term Variation of the Spin Period of a Magnetic Cataclysmic Variable, MU Camelopardalis

Long-Term Variation of the Spin Period of a Magnetic Cataclysmic Variable, MU Camelopardalis

The new period of the intermediate polar V709 Cas

Extensive photometry of the intermediate polar MU Cam: detection of a spin period change

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