Revisiting the mass- and radius-luminosity relations for FGK main-sequence stars

TL;DR

This study derives empirical mass and radius-luminosity relations for FGK main-sequence stars, incorporating metallicity and age, to improve stellar parameter estimations using eclipsing binary data and stellar evolution models.

Contribution

It provides new empirical relations that include age and metallicity effects, enhancing the accuracy of stellar mass and radius estimates for FGK stars.

Findings

Including age improves the fit quality, especially for mass.

Mass relation shows higher dispersion, likely due to stellar age effects.

Relations reproduce observed stellar parameters with 3.5% (mass) and 5.9% (radius) accuracy.

Abstract

Scaling relations are very useful tools for estimating unknown stellar quantities. Within this framework, eclipsing binaries are ideal for this goal because their mass and radius are known with a very good level of accuracy, leading to improved constraints on the models. We aim to provide empirical relations for the mass and radius as function of luminosity, metallicity, and age. We investigate, in particular, the impact of metallicity and age on those relations. We used a multi-dimensional fit approach based on the data from DEBCat, an updated catalogue of eclipsing binary observations such as mass, radius, luminosity, effective temperature, gravity, and metallicity. We used the {PARAM web interface for the Bayesian estimation of stellar parameters, along with} the stellar evolutionary code MESA to estimate the binary age, assuming a coeval hypothesis for both members. We derived the mass and radius-luminosity-metallicity-age relations using 56 stars, {with metallicity and mass in the range -0.34<[Fe/H]<0.27 and 0.66<M/M{_\odot}<1.8}. With that, the observed mass and radius are reproduced with an accuracy of 3.5% and 5.9%, respectively, which is consistent with the other results in literature. We conclude that including the age in such relations increases the quality of the fit, particularly in terms of the mass, as compared to the radius. On the other hand, as other authors have noted, we observed an higher dispersion on the mass relation than in that of the radius. We propose that this is due to a stellar age effect.