Spectroscopic and photometric study of the pulsating eclipsing binary HIP 28271

Abstract

We report the results of the detailed study of the single-lined eclipsing binary HIP 28271 with time-series high-resolution spectra and high-precision TESS photometry. The binary modeling indicates that HIP 28271 has a short orbital period of 2.7404254_-4e-7^+9e-7 days, with an eccentricity ofe_orb = 0.0062_-0.0013^+0.0006. Our light-curve analysis leads to the masses and radii for both components as follows: M₁ = 2.63_-0.10^+0.09 M_⊙, R₁ = 3.81_-0.07^+0.05 R_⊙, and M₂ = 0.86_-0.02^+0.02 M_⊙, R₂ = 0.84_-0.01^+0.01 R_⊙. Multiple frequency analyses of the residual light curves yields 23 significant pulsation signals, including ten independent frequencies. The pulsation periods and constants for the ten independent frequencies, and the physical parameters suggest that the primary component of HIP 28271 is a δ Sct pulsator.