Exploring the empirical instability strip for γ Dor-type stars in eclipsing binaries

This research paper has light-curve modelling, spectroscopy, and detailed asteroseismic studies for five detached eclipsing binaries with a gamma Dor component that have been found so far by the sky surveys. The objective is to study the pulsational characteristics of the oscillating stars of the systems, as well as to estimate their absolute parameters and their relation to the pulsational frequencies, and enrich the sample size of this kind of system, which has been relatively poor up today. The physical properties of these systems are compared with other similar cases and the locations of their components are plotted in the Hertzsprung-Russell (HR) diagrams. In order to discover the pulsation frequencies, the photometric data are analysed using eclipsing binary modelling methods and their residuals are subjected to Fourier analysis. Finally, we evaluated that there is a possible relationship between the pulsation periods of the primaries and the orbital period (P-orb), the force exerted per gram on the surface of the pulsating star (f/M-puls), and the fractional radius of the pulsating star (r(puls)) of the systems, using a sample of 39 eclipsing binary systems with gamma Dor type primaries. We utilized them to construct a unique observational gamma Dor instability strip, delineated by a lower limit of 6850 K at the red edge and an upper limit of 7360 K at the blue edge on the zero-age main sequence. The majority of 39 pure gamma Dor stars are located within the region that is covered by this observational strip.

Journal

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

Year

2025

Volume

538

Issue

2

Pages

726-744

ISSN

0035-8711

eISSN

1365-2966

DOI

10.1093/mnras/staf330

WoS UID

WOS:001439247700001