KIC 6220497: a new Algol-type eclipsing binary with multiperiodic pulsations

Lee, Jae Woo; Hong, Kyeongsoo; Koo, Jae‐Rim

doi:10.1093/mnras/stw1308

Cited by 23 publications

(23 citation statements)

References 48 publications

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“…In particular, KIC 06220497 (Lee et al 2016) and the four presented herein are oEA stars, nine of these are detached systems, while another three are still unclassified regarding their Roche geometry (see Liakos & Niarchos 2017, and references therein).…”

Section: Introductionmentioning

confidence: 93%

Asteroseismology ofKeplerAlgol-type oscillating eclipsing binaries

Liakos

2017

A&A

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Context. This research paper contains light curve modelling, spectroscopy and detailed asteroseismic studies for four out of five in total semidetached eclipsing binaries with a δ Scuti component, that have been detected to date through Kepler mission, namely KIC 06669809, KIC 10581918, KIC 10619109 and KIC 11175495. Aims. The goal is to study the pulsational characteristics of the oscillating stars of the systems as well as to estimate their absolute parameters and enrich the so far poor sample of this kind of systems. Methods. Ground based spectroscopic observations provide the means to estimate the spectral types of the primary components and to model the light curves with higher certainty. The photometric data are analysed using eclipsing binary modeling techniques, while Fourier analysis is applied on their residuals in order to reveal the pulsation frequency modes. Results. The results of analyses show that the primaries are pulsating stars of δ Scuti type and that all systems belong to the group of Algol type binaries with an oscillating star, namely oEA stars. The primaries of KIC 06669809, KIC 10581918, and KIC 10619109 pulsate in three, two, and five frequencies, respectively and in more than 200 other detected as combinations. The δ Scuti star of KIC 11175495 is the youngest and the fastest pulsator in binary systems that has ever been found and it oscillates in three main nonradial frequencies, while other 153 are also found as depended ones. Moreover, a comparison of their properties with other systems of the same type as well as with theoretical models of pulsating stars are also presented and discussed.

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Section: Introductionmentioning

confidence: 93%

Asteroseismology ofKeplerAlgol-type oscillating eclipsing binaries

Liakos

2017

A&A

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“…This synthesis was performed in a way similar to that for the pulsating EBs V404 Lyr ) and KIC 6220497 (Lee et al 2016a). The effective temperature of the hotter and more massive star was set to be 7590 K from the Kepler Input Catalogue (KIC; Kepler Mission Team 2009).…”

Section: Kepler Photometry and Light-curve Synthesismentioning

confidence: 99%

“…The signature of the tidally excited modes is the frequencies at multiples of the orbital frequency (Welsh et al 2011;Hambleton et al 2013). This paper is the fifth contribution in a series of detailed studies for pulsating stars in the Kepler EBs (Lee et al , 2016aLee 2016). We present that KIC 11401845 (R.A. 2000 = 19 h 25 m 11. s 275; decl.…”

Section: Introductionmentioning

confidence: 99%

KIC 11401845: An Eclipsing Binary with Multiperiodic Pulsations and Light-travel Time

Lee

Hong

Koo

2017

ApJ

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We report the Kepler photometry of KIC 11401845 displaying multiperiodic pulsations, superimposed on binary effects. Light-curve synthesis represents that the binary star is a short-period detached system with a very low mass ratio of q = 0.070 and filling factors of F 1 = 45 % and F 2 = 99 %. Multiple frequency analyses were applied to the light residuals after subtracting the synthetic eclipsing curve from the observed data. We detected 23 frequencies with signal to noise amplitude ratios larger than 4.0, of which the orbital harmonics (f 4 , f 6 , f 9 , f 15 ) in the low frequency domain may originate from tidally excited modes. For the high frequencies of 13.7−23.8 day −1 , the period ratios and pulsation constants are in the ranges of P pul /P orb = 0.020−0.034 and Q = 0.018−0.031 d, respectively. These values and the position on the Hertzsprung-Russell diagram demonstrate that the primary component is a δ Sct pulsating star. We examined the eclipse timing variation of KIC 11401845 from the pulsation-subtracted data and found a delay of 56±17 s in the arrival times of the secondary eclipses relative to the primary eclipses. A possible explanation of the time shift may be some combination of a light-travel-time delay of about 34 s and a very small eccentricity of e cos ω < 0.0002. This result represents the first measurement of the Rømer delay in non-compact binaries.

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“…In the observers' frame, this leads to multiplets spaced by (twice) the orbital frequency (Smeyers 2005). Such perturbed modes have been observed in a handful of stars (Lee et al 2016;Balona 2018;Bowman et al 2019;Southworth et al 2020;Jerzykiewicz et al 2020) and probably also in the eclipsing binary discussed by Hambleton et al (2013) as pointed out by Balona (2018).…”

Section: Ls04mentioning

confidence: 73%

Tidally perturbed pulsations in the pre-main sequence δ Scuti binary RS Cha

Steindl

Zwintz

Bowman

2021

A&A

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Context. Stellar components in binaries are subject to tidal forces which influence asteroseismic properties. Tidally pertubed pulsations have been reported for different objects but none of these are in their pre-main sequence phase of evolution. This makes RS Cha, consisting of two δ Scuti stars and with pulsational characteristics influenced by tidal effects, the first such object observed. Aims. We aim to investigate the pulsational properties of the eclipsing binary RS Cha in terms of the theory of tidally perturbed pulsations. Methods. Based on photometric time series obtained from the TESS satellite, we performed binary modelling using PHOEBE to interpret the binary light curve and to allow the investigation of the pulsations of both components in RS Cha. We modelled the detrended light curve with the superposition of linear modes. The frequencies were then interpreted as self excited modes perturbed by tidal forces. Results. We find evidence for tidally perturbed modes, which enables the identification of pulsation modes. RS Cha mainly exhibits dipole modes, while one prominent l = 2 or l = 3 mode is also inferred. The latter verifies previous results from spectroscopic time series. Conclusion. This work shows that RS Cha is an ideal candidate to test the theory of tidally perturbed pulsations within the framework of asteroseismic modelling. The identification of multiple pulsation modes using this theory is unprecedented and will be a keystone in the future of pre-main sequence asteroseismology. However, amplitude modulation caused by the changing light ratio during the orbital phase in an eclipsing binary also plays a significant role, which can complicate mode identification.

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KIC 6220497: a new Algol-type eclipsing binary with multiperiodic pulsations

Cited by 23 publications

References 48 publications

Asteroseismology ofKeplerAlgol-type oscillating eclipsing binaries

Asteroseismology ofKeplerAlgol-type oscillating eclipsing binaries

KIC 11401845: An Eclipsing Binary with Multiperiodic Pulsations and Light-travel Time

Tidally perturbed pulsations in the pre-main sequence δ Scuti binary RS Cha

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