A star’s rotation rate is difficult to estimate without surface inhomogeneities such as dark or bright spots. This paper presents asteroseismic results to determine the rotation rates of δ Sct-type pulsating primary stars in two eclipsing binary systems, AB Cas and OO Dra. After removing the binarity-induced light variations from archival TESS data and carefully examining the combination frequencies, we identified 12 independent frequencies for AB Cas and 11 frequencies for OO Dra, with amplitudes higher than ∼0.3 mmag, as δ Sct-type pulsation frequencies excited in each primary star. The theoretical frequencies for seismic analysis were obtained by fully considering rotation effects. Grid fitting for various stellar properties, such as mass, radius, metallicity, and rotation rate, yielded the best solutions for which the theoretical frequencies and stellar parameters agreed well with the observations. The rotation rate of the AB Cas primary was tightly constrained to 0.81 ± 0.01 day−1 (f rot/f orb = 1.11−0.02+0.01 ), which is slightly faster than the synchronized rotation. In contrast, the rotation rate of 0.63 ± 0.01 day−1 for the OO Dra primary is lower than the synchronous value of approximately 0.81 day−1. Subsynchronous rotation is uncommon in short-period binaries, and its physical mechanism is not yet well understood. Our results show that asteroseismology can be used to measure the rotation rate of fast-rotating δ Sct stars precisely and thus provide a valuable constraint on rotation–orbit synchronization in close binary systems.

https://iopscience.iop.org/article/10.3847/1538-4357/acc066/pdf

Asteroseismic Determination of Stellar Rotation: On Synchronization in the Close Eclipsing Binaries AB Cas and OO Dra

We present the ﬁrst evidence on the 𝛿 Sct type pulsations of the primary components of three eclipsing binaries IQ CMa, AW Men and W Vol in the TESS ﬁeld. A comprehensive investigation of the binary properties is conducted. The light curves of the systems are analysed and the frequency analyses are performed to residual data. The systems are compared to the binaries of the same morphological types, and the primaries are examined in contrast to the 𝛿 Sct type pulsators. The results show that the systems are oscillating eclipsing Algol-type systems.

/pdf/discovery-of-delta-sct-components-in-eclipsing-binary-1xlied9m.pdf

Discovery of $\delta$ Sct Components in Eclipsing Binary Systems IQ CMa, AW Men and W Vol

We present a new study of the Algol-type eclipsing binary system AS Eri based on the combination of the MOST and TESS light curves and a collection of very precise radial velocities obtained with the spectrographs HERMES operating at theMercator telescope, La Palma, and TCES operating at the Alfred Jensch telescope, Tautenburg. The primary component is an A3 V-type pulsating, mass-accreting star. We fitted the light and velocity data with the package PHOEBE, and determined the best-fitting model adopting the configuration of a semi-detached system. The orbital period has been improved using a recent (O-C) analysis and the phase shift detected between both light curves to the value 2.6641496 ± 0.0000001 days. The absence of any cyclic variation in the (O-C) residuals confirms the long-term stability of the orbital period. Furthermore, we show that the models derived for each light curve separately entail small differences, e.g. in the temperature parameter Teff,2. The high quality of the new solutions is illustrated by the residuals. We obtained the following absolute component parameters: L1 = 14.125 L , M1 = 2.014 M , R1 = 1.733 R , log g1 = 4.264, L2 = 4.345 L , M2 = 0.211 M , R2 = 2.19 R , log g2 = 3.078 with Teff,2/Teff,1 = 0.662 ± 0.002. Although the orbital period appears to be stable on the long term, we show that the light-curve shape is affected by a years-long modulation which is most probably due to the magnetic activity of the cool companion.

Updated modelling and refined absolute parameters of the oscillating eclipsing binary AS Eri

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Updated modelling and refined absolute parameters of the oscillating eclipsing binary AS Eri