BD ANDROMEDAE: A NEW SHORT-PERIOD RS CVn ECLIPSING BINARY STAR WITH A DISTANT TERTIARY BODY IN A HIGHLY ECCENTRIC ORBIT

Kim, Chun-Hwey; Song, Mi-Hwa; Yoon, Joh-Na; Han, Wonyong; Jeong, Min-Ji

doi:10.1088/0004-637x/788/2/134

Cited by 15 publications

(34 citation statements)

References 85 publications

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“…However, for further discussion on the cause of the period change, the evolution of the binary system, and so on, we have estimated the absolute physical quantities of NSVS 1461538 indirectly, as listed in Table 7. The method to estimate these quantities is described in detail in Kim et al (2014). As discussed in Section 3, the period variation of 5.6 yr can be explained by a magnetic model of Applegate (1992) or the light-time effect due to a tertiary body.…”

Section: Discussionmentioning

confidence: 99%

“…All the raw CCD images obtained are pre-processed by compensating for bias, dark, and flat using the IRAF/CCDPRO package and post-processed using IRAF/DAOPHOT. Further details of raw data processing are described in Kim et al (2014).…”

Section: Observation and Reductionmentioning

confidence: 99%

“…Recently, we have been making photometric observations of close binary stars whose photometric characteristics are not well known (Kim & Jeong 2012;Kim et al 2014). As one task of the project, we have observed NSVS 1461538 (2MASS J23102148+5859170, SWASP J231021.48+585917.2) and its neighboring PV Cas at the same time.…”

Section: Introductionmentioning

confidence: 99%

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The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

Kim¹,

Kim²,

Song³

et al. 2016

Journal of Astronomy and Space Sciences

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Section: Discussionmentioning

confidence: 99%

Section: Observation and Reductionmentioning

confidence: 99%

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The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

Kim¹,

Kim²,

Song³

et al. 2016

Journal of Astronomy and Space Sciences

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“…Telescope tracking is performed via a servo motor control. More details of this telescope was described by Kim et al (2014).…”

Section: Observationsmentioning

confidence: 99%

Photometric Defocus Observations of Transiting Extrasolar Planets

Hinse¹,

Han

Yoon³

et al. 2015

Journal of Astronomy and Space Sciences

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We have carried out photometric follow-up observations of bright transiting extrasolar planets using the CbNUOJ 0.6m telescope. We have tested the possibility of obtaining high photometric precision by applying the telescope defocus technique allowing the use of several hundred seconds in exposure time for a single measurement. We demonstrate that this technique is capable of obtaining a rootmean-square scatter of order sub-millimagnitude over several hours for a V ∼ 10 host star typical for transiting planets detected from ground-based survey facilities. We compare our results with transit observations with the telescope operated in in-focus mode. High photometric precision is obtained due to the collection of a larger amount of photons resulting in a higher signal compared to other random and systematic noise sources. Accurate telescope tracking is likely to further contribute to lowering systematic noise by probing the same pixels on the CCD. Furthermore, a longer exposure time helps reducing the effect of scintillation noise which otherwise has a significant effect for small-aperture telescopes operated in in-focus mode. Finally we present the results of modelling four light-curves for which a root-mean-square scatter of 0.70 to 2.3 milli-magnitudes have been achieved.

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“…Only recently, Sipahi & Dal (2014) obtained CCD BV R photometry of the system and found that (i) the true orbital period is two times longer than determined previously, (ii) the mass ratio of the eclipsing binary is about 0.97, (iii) minima times show a cyclic variability indicating presence of a third body on about 9.6-year orbit, and (iv) light variation outside the primary eclipse may result from γ Dor oscillations of the primary component. Subsequently Kim et al (2014) analyzed extensive new BV R photometry as well as published timing data. The data analysis confirmed periodic orbital period variations indicating a third component revolving on a highly eccentric orbit with e ∼ 0.76.…”

Section: Introductionmentioning

confidence: 99%

Close eclipsing binary BD And: a triple system

Pribulla¹,

Hambálek²,

Guenther³

et al. 2020

caosp

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BD And is a fairly bright (V = 10.8), active and close (P ∼ 0.9258 days) eclipsing binary. The cyclic variability of the apparent orbital period as well as third light in the light curves indicate the presence of an additional late-type component. The principal aim is the spectroscopic testing of the third-body hypothesis and determination of absolute stellar parameters for both components of the eclipsing binary. First medium and high-resolution spectroscopy of the system was obtained. The broadening-function technique appropriate for heavily-broadened spectra of close binaries was used. The radial velocities were determined fitting the Gaussian functions and rotational profiles to the broadening functions. A limited amount of photometric data has also been obtained. Although the photometric observations were focused on the obtaining the timing information, a cursory light-curve analysis was also performed. Extracted broadening functions clearly show the presence of a third, slowly-rotating component. Its radial velocity is within error of the systemic velocity of the eclipsing pair, strongly supporting the physical bond. The observed systemic radial-velocity and third-component changes do not support the 9 year orbit found from the timing variability. Masses of the components of the eclipsing pair are determined with about 0.5% precision. Further characterization of the system would require long-term photometric and spectroscopic monitoring.

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BD ANDROMEDAE: A NEW SHORT-PERIOD RS CVn ECLIPSING BINARY STAR WITH A DISTANT TERTIARY BODY IN A HIGHLY ECCENTRIC ORBIT

Cited by 15 publications

References 85 publications

The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

Photometric Defocus Observations of Transiting Extrasolar Planets

Close eclipsing binary BD And: a triple system

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