Comprehensive analysis of southern eclipsing systems with pulsating components: The cases of HM Pup, V632 Sco and TT Vel

TL;DR

This study conducts a detailed multi-faceted analysis of three southern semi-detached eclipsing binaries with pulsating components, combining photometry, spectroscopy, and theoretical modeling to understand their properties and pulsation modes.

Contribution

It provides the first comprehensive analysis of HM Pup, V632 Sco, and TT Vel, including pulsation mode identification and orbital period variation mechanisms.

Findings

Primaries are δ Scuti type pulsators.

Mass flow from secondary components observed.

Orbital period modulations linked to specific mechanisms.

Abstract

This work presents an extensive analysis of the properties of three southern semi-detached eclipsing binaries hosting a pulsating component, namely HM Pup, V632 Sco, and TT Vel. Systematic multi-filtered photometric observations were obtained using telescopes located in Australia and Chile mostly between 2018-2021. These observations were combined with data from the Transiting Exoplanet Survey Satellite (TESS) mission for a detailed analysis of pulsations. Spectral types and radial velocities were determined from spectra obtained with the Australian National University's 2.3 m telescope and Wide Field Spectrograph. The data are modelled and the absolute parameters of all components are derived. The light curve residuals are further analysed using Fourier transformation techniques for the determination of the pulsation frequencies. Using theoretical models, the most probable modes of the principal oscillations are also identified. Eclipse-timing variation analysis is also made for all systems and the most likely mechanisms modulating the orbital period are proposed. The physical properties of these systems are compared with other similar cases and the locations of their components are plotted in the M-R and HR diagrams. Finally, the pulsational properties of the oscillating components are compared with currently known systems of this type within the orbital-pulsation period and log g-pulsation period diagrams. These systems are identified as oEA stars by definition, with the primaries to be pulsating stars of $\delta$ Scuti type, while evidence of mass flow from the evolved secondary components is present in their Na I D spectra.