Exploring Detached Eclipsing Binary Systems from TESS Observations: Insights into OBA-type Systems and Orbital Circularization

TL;DR

This paper provides detailed photometric solutions for 181 detached eclipsing binary systems observed by TESS, offering new insights into OBA-type systems, orbital parameters, and the orbital circularization process, with implications for tidal interaction theories.

Contribution

It introduces the first comprehensive photometric solutions for 172 well-detached eclipsing binaries from TESS data, and compares observed circularization periods with theoretical predictions.

Findings

Photometric solutions for 172 systems are unprecedented.

Identified a primary radius fraction of 0.266 for radiative envelope stars.

Determined a circularization period of 5.762 days, challenging existing theories.

Abstract

This study presents photometric solutions for a carefully selected sample of 181 detached eclipsing binary systems recently observed by the Transiting Exoplanet Survey Satellite (TESS) mission. Our findings contribute to discussions about OBA-type systems and the orbital circularization influenced by tidal interactions. The results encompass crucial parameters, including the sum of radii fraction ($r_{\rm a}\,+\,r_{\rm b}$), radii ratio ($k$), orbital inclination ($i$), surface brightness ratio ($J$), and combinations of the longitude of the periastron and orbital eccentricity ($e\,\sin\,\omega$ and $e\,\cos\,\omega$). Geometric light curve fitting is performed using version 43 of the {\sc jktebop} code, serving as the primary tool for determining orbital elements and physical ratios. Careful uncertainty estimates for these findings are derived through bootstrap simulations. This work introduces unprecedented photometric solutions for 172 well-detached eclipsing systems, while the results for the remaining nine systems exhibit excellent agreement with those previously reported in the literature. Additionally, a critical primary radius fraction ($R_{\rm a}/a$) of 0.266 is identified for our sample of radiative envelope stars, consistent with observational and theoretical findings in the literature. Finally, we determine a circularization period of 5.762 days based on a function from the literature, revealing a discrepancy with Zahn's theory for hot stars.