A comprehensive study of δ Scuti-type pulsators in eclipsing binaries: Oscillating eclipsing Algols

¹ Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences ul. Rabiańska 8 87-100 Toruń, Poland
² Villanova University, Dept. of Astrophysics and Planetary Sciences 800 East Lancaster Avenue Villanova PA 19085, USA
³ Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences ul. Bartycka 18 00-716 Warszawa, Poland
⁴ Astrophysics Group, Keele University Staffordshire ST5 5BG, U.K.

^★ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.

Received: 28 February 2025
Accepted: 4 November 2025

Abstract

Eclipsing double-lined spectroscopic binaries (SB2s) hosting δ Scuti-type pulsators offer a unique laboratory for simultaneously constraining stellar geometry and interior structure. In this study, we present a comprehensive analysis of five oscillating eclipsing Algol (oEA) binaries. By combining high-precision, short-cadence TESS photometry with multi-epoch high-resolution spectroscopy, we were able to derive precise stellar and orbital parameters. The frequency power spectra were obtained using residuals from binary modelling. We further investigated the evolutionary history of these systems using a grid of MESA binary evolution simulations. Our analysis suggests that the systems must have undergone either case A or case B mass transfer, with the primary components repositioned in the Hertzsprung–Russell (HR) diagram and now pulsating in the δ Scuti regime, while the cooler secondaries are underluminous and inflated, filling their Roche lobes. This study contributes to the growing catalog of well-characterised oEA systems and our understanding of the effects of mass-transfer on the fate of these short-period binaries.