Two-Color CCD Photometry of the Intermediate Polar 1rxs J180340.0+401214

Андронов, И. Л.; Kim, Yonggi Kim; Yoon, Joh-Na; Breus, V. V.; Smecker-Hane, T.; Chinarova, L. L.; Han, Wonyong

doi:10.5303/jkas.2011.44.3.89

Cited by 3 publications

(4 citation statements)

References 19 publications

(12 reference statements)

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“…Contrary to previous studies of the same field (cf. Andronov et al 2011) with smaller field, these images contained this new variable. The vari-able was registered as VSX J180243.9+400331 (hereafter VSX1802).…”

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confidence: 83%

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Phenomenological Modeling of Newly Discovered Eclipsing Binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331

Андронов¹,

Kim²,

Kim³

et al. 2015

Journal of Astronomy and Space Sciences

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During processing the observations of the intermediate polar 1RXS J180340.0+401214, obtained 26.05.2012 at the 60-cm telescope of the Mt. Suhora observatory (Krakow, Poland), variability of 2MASS J18024395 +4003309 was discovered. As this object was not listed in the General Catalogue of Variale Stars or Variable Stars Index, we registered it as VSX J180243.9+400331. Additionally we used 189 separate observations from the Catalina Sky Survey spread over 7 years. The periodogram analysis yields the period of 0 d .3348837±0 d .0000002.The object was classified as the Algol-type eclipsing binary with a strong effect of ellipticity. The depths of the primary and secondary minima are nearly identical, which corresponds to a brightness (and maybe) mass ratio close to 1. The statistically optimal degree of the trigonometric polynomial n=4. The most recent minimum occurred at HJD 2456074.4904. The brightness range from our data is 16.56-17.52 (V), 16.18-17.08 (R).The NAV (New Algol Variable) algorithm was applied for statistically optimal phenomenological modeling and determination of corresponding parameters.

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confidence: 83%

“…North is up and West is left. The numeration of comparison stars is as in Andronov et al (2011), except the star 13. with corresponding error estimates 0.013, 0.025, 0.020, 0.039, 0.018, 0.034, 0.021, 0.045. For the color index, the deviation of the coefficient from unity exceeds 4s and thus is to be taken into account.…”

mentioning

confidence: 99%

Phenomenological Modeling of Newly Discovered Eclipsing Binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331

Андронов¹,

Kim²,

Kim³

et al. 2015

Journal of Astronomy and Space Sciences

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“…Two-Color CCD Photometry of the Intermediate Polar 1RXS J180340. 0 +401214 showed a remarkably stable period (Andronov et al (2011)).…”

Section: Intermediate Polarsmentioning

confidence: 94%

Astroinformatics: Statistically Optimal Approximations of Near-Extremal Parts with Application to Variable Stars

Андронов

Andrych

Chinarova

et al. 2020

ComBAO

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The software MAVKA is described, which was elaborated for statistically optimal determination of the characteristics of the extrema of 1000+ variable stars of different types, mainly eclipsing and pulsating. The approximations are phenomenological, but not physical. As often, the discovery of a new variable star is made on time series of a single-filter (single-channel) data, and there is no possibility to determine parameters needed for physical modelling (e.g. temperature, radial velocities, mass ratio of binaries). Besides classical polynomial approximation "AP" (we limited the degree of the polynomial from 2 to 9), there are realized symmetrical approximations (symmetrical polynomials "SP", "wall-supported" horizontal line "WSL" and parabola "WSP", restricted polynomials of non-integer order based on approximations of the functions proposed by Andronov (2012) and Mikulasek (2015) and generally asymmetric functions (asymptotic parabola "AP", parabolic spline "PS", generalized hyperbolic secant function "SECH" and "log-normal-like" "BSK"). This software is a successor of the "Observation Obscurer" with some features for the variable star research, including a block for "running parabola" "RP" scalegram and approximation. Whereas the RP is oriented on approximation of the complete data set. MAVKA is pointed to parts of the light curve close to extrema (including total eclipses and transits of stars and exoplanets). The functions for wider intervals, covering the eclipse totally, were discussed in Andronov (2017). Global and local approximations are reviewed in Andronov (2020). The software is available at http://uavso.org.ua/mavka and https://katerynaandrych.wixsite.com/mavka. We have analyzed the data from own observations, as well as from monitoring obtained at ground-based and space (currently, mainly, TESS) observatories. It may be used for signals of any nature.

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“…The optical monitoring of MCVs has been performed in Korea since 1995 using domestic telescopes and as a part of "Inter-Longitude Astronomy" campaign (Andronov et al 2010), international observation monitoring was conducted and the analysis results have been reported (Andronov et al 2008(Andronov et al , 2011(Andronov et al , 2015Kim et al 2004Kim et al , 2005aKim et al , 2005bKim et al , 2009Yun et al 2011) While DO Dra, one of the target stars of ILA campaign, shows variable amplitude and ejection behavior with indeterminable periods, various periods and QPO phenomena obtained from photometric observation data of DO Dra have been analyzed and the results are presented in this study.…”

Section: Introductionmentioning

confidence: 99%

Quasi-Periodic Oscillation of a Magnetic Cataclysmic Variable, DO Draconis

Han¹,

Kim²,

Андронов³

et al. 2017

Journal of Astronomy and Space Sciences

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In this paper, analysis results of the photometric data of DO Dra will be presented. DO Dra had been observed with 1 m LOAO telescope and 0.6 m CBNUO telescope from 2005 through 2014. The data shows kind of periodic oscillation behavior in the orbital period and also in the spin period. It has been found that these QPOs are not observed always and that the periods vary from 30 min to 80 min. We also found that the period variation seems to repeat itself with the period of 13.5 days. It is essential to monitor this object in the future as well as to carry out model calculation in order to have better understanding of these QPO phenomena.

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Two-Color CCD Photometry of the Intermediate Polar 1rxs J180340.0+401214

Cited by 3 publications

References 19 publications

Phenomenological Modeling of Newly Discovered Eclipsing Binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331

Phenomenological Modeling of Newly Discovered Eclipsing Binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331

Astroinformatics: Statistically Optimal Approximations of Near-Extremal Parts with Application to Variable Stars

Quasi-Periodic Oscillation of a Magnetic Cataclysmic Variable, DO Draconis

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