Determination of tidal distortion in the eclipsing binary system V621 Cen by means of deviations from the third Kepler law

TL;DR

This study estimates the tidal distortion parameter of V621 Cen's secondary star by comparing observed and Keplerian orbital periods, providing insights into stellar deformation in eclipsing binaries.

Contribution

It introduces a method to determine tidal distortion without relying on periastron precession, applicable to circular orbit systems.

Findings

Tidal distortion parameter k_m = -1.5 +/- 0.6

Method applicable to circular orbit binaries

Provides a new approach to stellar deformation analysis

Abstract

In this paper we determine the tidal distortion parameter k_m of the secondary partner (mass loser) of the semi-detached eclipsing binary system V621 Cen by comparing the phenomenologically determined orbital period P_b=3.683549(11) d to the Keplerian one P^Kep computed with the values of the relevant system's parameters determined independently of the third Kepler law itself. Our result is k_m = -1.5 +/- 0.6. Using the periastron precession, as traditionally done with other eclipsing binaries in eccentric orbits, would have not been possible because of the circularity of the V621 Cen path.