[논문]POORLY STUDIED ECLIPSING BINARIES IN THE FIELD OF DO DRACONIS: V454 DRA AND V455 DRA

Kim, Yonggi; Andronov, Ivan L.; Andrych, Kateryna D.; Yoon, Joh-Na; Han, Kiyoung; Chinarova, Lidia L.

doi:10.5303/jkas.2020.53.2.43

POORLY STUDIED ECLIPSING BINARIES IN THE FIELD OF DO DRACONIS: V454 DRA AND V455 DRA 원문보기

Journal of the Korean astronomical society = 천문학회지, v.53 no.2, 2020년, pp.43 - 48

Kim, Yonggi (Chungbuk National University Observatory, Chungbuk National University) , Andronov, Ivan L. (Department "Mathematics, Physics and Astronomy", Odessa National Maritime University) , Andrych, Kateryna D. (Department "Mathematics, Physics and Astronomy", Odessa National Maritime University) , Yoon, Joh-Na (Chungbuk National University Observatory, Chungbuk National University) , Han, Kiyoung (Chungbuk National University Observatory, Chungbuk National University) , Chinarova, Lidia L. (Department "Mathematics, Physics and Astronomy", Odessa National Maritime University)

Abstract ▼ AI-Helper

We report an analysis of two poorly studied eclipsing binary stars, GSC 04396-00605 and GSC 04395-00485 (recently named V455 Dra and V454 Dra, respectively). Photometric data of the two stars were obtained using the 1-m Korean telescope of the LOAO operated by KASI while monitoring the cataclysmic variable DO Dra in the frame of the Inter-Longitude Astronomy (ILA) project. We derived periods of 0.434914 and 0.376833 days as well as initial epochs JD 2456480.04281 and JD 2456479.0523, respectively, more accurate than previously published values by factors 9 and 6. The phenomenological characteristics of the mean light curves were determined using the New Algol Variable (NAV) algorithm. The individual times of maxima/minima (ToM) were determined using the newly developed software MAVKA, which outputs accurate parameters using "asymptotic parabola" approximations. The light curves were approximated using phenomenological and physical models. In the NAV algorithm, the phenomenological parameters are well determined. We derived physical parameters using the Wilson-Devinney model. In this model, the best-fit parameters are highly correlated, thus some of them were fixed to reasonable values. For both systems, we find evidence for the presence of a cool spot and estimate its parameters. Both systems can be classified as overcontact binaries of EW type.

주제어

표/그림 (9)

그림 Figure 1. The phase light curve of V454 Dra together with the best-fit NAV model (continuous line following the data).
그림 Figure 2. The phase light curve of V455 Dra together with the best-fit NAV model (continuous line following the data).
그림 Figure 3. The phase light curve of V454 Dra with the best-fit Wilson-Devinney model.
그림 Figure 4. The phase light curve of V455 Dra with the best-fit Wilson-Devinney model.
그림 Figure 5. Model of V454 Dra with its cool spot (red area), as seen at an orbital phase φ = 0.74.
그림 Figure 6. Same as Figure 5 for V455 Dra, as seen at φ = 0.24.
표 Table 1 Parameter values determined by phenomenological modeling
표 Table 2 Moments of individual maxima and minima
표 Table 3 Parameter values derived from physical modeling

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제안 방법

Photometric time series for two poorly known binary stars, V454 Dra and V455 Dra, were analyzed using phenomenological approximations of the complete phase light curve (using the trigonometric polynomial and NAV algorithms), as well as individual time series around maxima and minima (using the “asymptotic parabola” algorithm implemented in the recently developed software MAVKA), and a database containing almost 70 moments was compiled.

대상 데이터

The telescope is equipped with a 2048 × 2048 pixel CCD camera with a pixel scale of 0.64 arcsec/pixel and a field of view (FOV) of 22'.2 × 22'.2.

이론/모형

(More details may be found in the monograph by Kallrath & Milone 2009.) The algorithm is based on a Roche model geometry for the construction of a binary system and uses Monte Carlo simulations to specify physical parameters and construct a model light curve. The WD-code allows to simulate different types of eclipsing systems from contact systems to exoplanet transits
We also applied physical modeling to our data using the Wilson-Devinney algorithm. The set of physical parameters which were determined should be regarded as an initial approximation, which may be improved using possible further spectral observations (to determine mass ratios and temperatures) or well-calibrated multi-color photometry (to determine temperatures).

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