KIC 8553788: A pulsating Algol with an extreme mass ratio

Liakos, A.

doi:10.1051/0004-6361/201832639

Cited by 13 publications

(14 citation statements)

References 52 publications

(89 reference statements)

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“…As described in previous works (Liakos 2017(Liakos , 2018, the analyses of EBs observed by Kepler LCs require some special attention due to light variations between successive LCs. Therefore, in order to avoid a super simplified model that includes all data points folded into the P orb , the method based on one model per LC (using normal points) or one model per a group of successive LCs folded into the P orb was followed.…”

Section: Light-curve Modelling and Absolute Parameters Calculationmentioning

confidence: 99%

“…The present paper is a continuation of the systematic study on EBs with a δ Scuti component (see also Liakos & Niarchos 2009Liakos & Cagaš 2014;Liakos 2017Liakos , 2018 and aims to enrich the current sample of this kind of systems. For KIC 10686876 only preliminary results have been published regarding its dominant pulsational frequencies (Liakos & Niarchos 2017).…”

Section: Introductionmentioning

confidence: 99%

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Asteroseismology of twoKeplerdetached eclipsing binaries

Liakos

2020

A&A

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The present work contains light curve, spectroscopic, and asteroseismic analyses for KIC 04851217 and KIC 10686876. These systems are detached eclipsing binaries hosting a pulsating component of δ Scuti type and have been observed with the unprecedented accuracy of the Kepler space telescope. Using ground-based spectroscopic observations, the spectral types of the primary components of the systems were estimated as A6V and A5V for KIC 04851217 and KIC 10686876, respectively, with an uncertainty of one subclass. The present spectral classification, together with literature radial velocity curves, were used to model the light curves of the systems and, therefore, to calculate the absolute parameters of their components with a higher degree of certainty. The photometric data were analysed using standard eclipsing binary modeling techniques, while their residuals were further analysed using Fourier transformation techniques to extract the pulsation frequencies of their host δ Scuti stars. The oscillation modes of the independent frequencies were identified using theoretical models of δ Scuti stars. The distances of the systems were calculated using the relation between the luminosity and the pulsation period for δ Scuti stars. Here, the physical and the oscillation properties of the pulsating components of these systems are discussed and compared with others of the same type. Moreover, using all the currently known cases of δ Scuti stars in detached binaries, updated correlations between orbital and dominant pulsation periods and between log g and pulsation periods are derived. It can concluded that the proximity of the companion plays significant role in the evolution of the pulsational frequencies.

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Section: Light-curve Modelling and Absolute Parameters Calculationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Asteroseismology of twoKeplerdetached eclipsing binaries

Liakos

2020

A&A

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“…The companion is usually a low-mass star filling or nearly-filling its Roche lobe, depending on whether the mass transfer process is finished or not. To name a few, AS Eri (Mkrtichian et al, 2004), KIC 4739791 (Lee et al, 2016), KIC 8553788 (Liakos, 2018), V392 Orionis (Hong et al, 2019), KIC 10736223 (Cheng et al, 2020). found the period spacing pattern of dipole g modes in mass-accreting γ Dor star in KIC 9592855.…”

Section: Mass-accreting Pulsatorsmentioning

confidence: 99%

Asteroseismology of Close Binary Stars: Tides and Mass Transfer

Guo

2021

Front. Astron. Space Sci.

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The study of stellar oscillations allows us to infer the properties of stellar interiors. Meanwhile, fundamental parameters such as mass and radius can be obtained by studying stars in binary systems. The synergy between binarity and asteroseismology can constrain the parameter space of stellar properties and facilitate the asteroseismic inference. On the other hand, binarity also introduces additional complexities such tides and mass transfer. From an observational perspective, we briefly review the recent advances in the study of tidal effects on stellar oscillations, focusing on upper main sequence stars (F-, A-, or OB- type). The effect can be roughly divided into two categories. The first one concerns the tidally excited oscillations (TEOs) in eccentric binaries where TEOs are mostly due to resonances between dynamical tides and gravity modes of the star. TEOs appear as orbital-harmonic oscillations on top of the eccentric ellipsoidal light curve variations (the “heartbeat” feature). The second category is regarding the self-excited oscillations perturbed by static tides in circularized and synchronized close binaries. It includes the tidal deformation of the propagation cavity and its effect on eigenfrequencies, eigenfunctions, and the pulsation alignment. We list binary systems that show these two types of tidal effect and summarize the orbital and pulsation observables. We also discuss the theoretical approaches used to model these tidal oscillations and relevant complications such as non-linear mode coupling and resonance locking. Further information can be extracted from the observations of these oscillations which will improve our understanding of tides. We also discuss the effect of mass transfer, the extreme result of tides, on stellar oscillations. We bring to the readers' attention: (1) oscillating stars undergoing mass accretion (A-, F-, and OB type pulsators and white dwarfs), for which the pulsation properties may be changed significantly by accretion; (2) post-mass transfer pulsators, which have undergone a stable or unstable Roche-Lobe overflow. These pulsators have great potential in probing detailed physical processes in stellar interiors and mass transfer, as well as in studying the binary star populations.

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“…As described in the previous works (Liakos 2017(Liakos , 2018, the analyses of EBs observed by Kepler LCs need some special attention due to light variations between successive LCs. Therefore, in order to avoid a super simplified model including all data points folded into the P orb , the method of one model per LC (using normal points) or one model per a group of successive LCs folded into the P orb was followed.…”

Section: Light Curve Modelling and Absolute Parameters Calculationmentioning

confidence: 99%

“…The present paper is a continuation of the systematic study on EBs with a δ Scuti component (see also Liakos & Niarchos 2009, 2013Liakos & Cagaš 2014;Liakos & Niarchos 2016;Liakos 2017Liakos , 2018 and aims to enrich the current sample of this kind of systems. Preliminary results have been published for KIC 10686876 (Liakos & Niarchos 2017), regarding its dominant pulsational frequencies, and together with KIC 04851217 were selected for detailed analyses for first time.…”

Section: Introductionmentioning

confidence: 99%

Asteroseismology of two Kepler detached eclipsing binaries

Liakos

2020

Preprint

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The present work contains light curve, spectroscopic and asteroseismic analyses for KIC 04851217 and KIC 10686876. These systems are detached eclipsing binaries hosting a pulsating component of δ Scuti type and have been observed with the unprecedented accuracy of the Kepler space telescope. Using ground based spectroscopic observations, the spectral types of the primary components of the systems were estimated as A6V and A5V for KIC 04851217 and KIC 10686876, respectively, with an uncertainty of one subclass. The present spectral classification together with literature radial velocities curves were used to model the light curves of the systems and, therefore, to calculate the absolute parameters of their components with higher certainty. The photometric data were analysed using standard eclipsing binary modeling techniques, while their residuals were further analysed using Fourier transformation techniques in order to extract the pulsation frequencies of their host δ Scuti stars. The oscillation modes of the independent frequencies were identified using theoretical models of δ Scuti stars. The distances of the systems were calculated using the relation between the luminosity and the pulsation period for δ Scuti stars. The physical and the oscillation properties of the pulsating components of these systems are discussed and compared with others of the same type. Moreover, using all the currently known cases of δ Scuti stars in detached binaries, updated correlations between orbital and dominant pulsation periods and between log g and pulsation periods were derived. It was found that the proximity of the companion plays significant role to the evolution of the pulsational frequencies.

show abstract

KIC 8553788: A pulsating Algol with an extreme mass ratio

Cited by 13 publications

References 52 publications

Asteroseismology of twoKeplerdetached eclipsing binaries

Asteroseismology of twoKeplerdetached eclipsing binaries

Asteroseismology of Close Binary Stars: Tides and Mass Transfer

Asteroseismology of two Kepler detached eclipsing binaries

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