Abstract
The present work concerns the Asteroseismology of the Kepler-detached eclipsing binary KIC 8504570. Particularly, it focuses on the pulsational behaviour of the oscillating component of this system and the estimation of its physical parameters in order to enrich the so far poor sample of systems of this kind. Using spectroscopic observations, the spectral type of the primary component was determined and used to create accurate light curve models and estimate its absolute parameters. The light curve residuals were subsequently analysed using Fourier transformation techniques to obtain the pulsation models. Theoretical models of δ Scuti stars were employed to identify the oscillation modes of the six detected independent frequencies of the pulsator. In addition, more than 385 combination frequencies were also detected. The absolute and the pulsational properties of the δ Scuti star of this system are discussed and compared with all the currently known similar cases. Moreover, using a recent(empirical) luminosity–pulsation period relationship for δ Scuti stars, the distance of the system was estimated.
Highlights
The δ Scuti stars are short-period and multiperiodic pulsating variables
The differences of spectral line depths between each standard star and the target star were compared via sums of squared residuals in each case, with the least squares sums indicating the best fit. This method is quite efficient in cases of eclipsing binaries (EBs) with large luminosity differences between their components, because the total spectrum is practically dominated by the light of the primary star
The primary component was identified as a δ Scuti star and its pulsational characteristics were accurately determined
Summary
The δ Scuti stars are short-period and multiperiodic pulsating variables. In general, they oscillate in radial and low-order non-radial pulsations due to κ-mechanism [1,2]. For the aforementioned reasons, in the absence of radial velocity curves, the least-squares minimisation technique has to be applied to the photometric data in order to estimate the parameters of the components Another powerful tool of the EBs is the “eclipse timing variations” (ETV) method, which allows one to detect mechanisms (e.g., mass transfer, tertiary component, etc.; c.f. Budding and Demircan [17]-ch. and Borkovits et al [18] and references therein) that modulate the orbital period. The subject of δ Scuti stars in EBs is extremely interesting because it combines two totally different topics of astrophysics and provides the means for remarkable results On one hand, these systems host an oscillating component, whose pulsational properties are directly measurable by analysing photometric/spectroscopic data.
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