A γ Doradus candidate in eclipsing binary BD And?

Sipahi, E.; Dal, H. A.

doi:10.1016/j.newast.2013.06.001

Cited by 5 publications

(5 citation statements)

References 19 publications

(22 reference statements)

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“…The existence of a third component on a long-period orbit was first indicated by the timing variability and third light in the LC modeling (see Sipahi & Dal, 2014). Our new spectroscopy conclusively shows the presence of an additional component.…”

Section: Third Component and The Outer Orbitsupporting

confidence: 70%

“…BD And was identified as a ROSAT source by Shaw et al (1996), and it was detected by Swift (Evans et al, 2013) and twice in the course of the XMM-Newton Slew Survey (XMM-SSC, 2018), indicating that the source has a high level of magnetic activity. 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.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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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Section: Third Component and The Outer Orbitsupporting

confidence: 70%

Section: Introductionmentioning

confidence: 99%

Close eclipsing binary BD And: a triple system

Pribulla¹,

Hambálek²,

Guenther³

et al. 2020

caosp

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“…Aerts et al (2002) report the detection of δ Sct pulsations in the 1.15-day orbit ellipsoidal binary XX Pyx. Dal & Sipahi (2013) report the detection of δ Sct oscillations in the 0.69-day orbit ellipsoidal binary V1464 Aql, and Sipahi & Dal (2014) orbit near-contact binary V392 Ori. From the present study, the ten systems displaying γ Dor and/or δ Sct with P orb < 0.5 day are odd as no oscillations have been detected so far, as far as we know, in such short period systems.…”

Section: Classical Pulsatorsmentioning

confidence: 99%

Systematic search for stellar pulsators in the eclipsing binaries observed byKepler

Gaulme

Guzik

2019

A&A

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Eclipsing binaries (EBs) are unique targets for measuring precise stellar properties and constrain stellar evolution models. In particular, it is possible to measure at the percent level masses and radii of both components of a double-lined spectroscopic EB. Since the advent of high-precision photometric space missions (MOST, CoRoT, Kepler, BRITE, TESS), the use of stellar pulsation properties to infer stellar interiors and dynamics constitutes a revolution for low-mass star studies. The Kepler mission has led to the discovery of thousands of classical pulsators such as δ Scuti and solar-like oscillators (main sequence and evolved), but also almost 3000 EBs with orbital periods shorter than 1100 days. We report the first systematic search for stellar pulsators in the entire Kepler eclipsing binary catalog. The focus is mainly aimed at discovering δ Scuti, γ Doradus, red giant, and tidally excited pulsators. We developed a data inspection tool (DIT) that automatically produces a series of plots from the Kepler light-curves that allows us to visually identify whether stellar oscillations are present in a given time series. We applied the DIT to the whole Kepler eclipsing binary database and identified 303 systems whose light curves display oscillations, including 163 new discoveries. A total of 149 stars are flagged as δ Scuti (100 from this paper), 115 stars as γ Doradus (69 new), 85 stars as red giants (27 new), 59 as tidally excited oscillators (29 new). There is some overlap among these groups, as some display several types of oscillations. Despite many of these systems are likely to be false positives, i. e., when an EB light curve is blended with a pulsator, this catalog gathers a vast sample of systems that are valuable for a better understanding of stellar evolution.

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“…Its properties are relatively poorly known compared to those of other short-period binaries. There is no spectroscopic study for BD And in the literature [40]. The photometric lightcurves of BD And in the BVR-bands were observed in 2008 and 2009 [40].…”

mentioning

confidence: 99%

“…There is no spectroscopic study for BD And in the literature [40]. The photometric lightcurves of BD And in the BVR-bands were observed in 2008 and 2009 [40]. Using these observations authors determined the photometric solution of BD And.…”

mentioning

confidence: 99%