What are the temperatures of T Tauri stars? - Constraints from coeval formation of young eclipsing binaries

TL;DR

This paper introduces a method to constrain the effective temperatures of young eclipsing binary stars by using coeval formation assumptions and compares models to observed parameters, revealing inconsistencies in current models.

Contribution

The paper extends existing methods to jointly analyze stellar parameters and coevality, providing a new approach to constrain temperatures of young binary stars.

Findings

V1174 Ori A has dwarf-like temperatures at 9 Myrs

Current models do not produce coeval solutions in mass, radius, and temperature

The method confirms temperature constraints for some binaries but not all.

Abstract

We show how the assumption of coeval formation can be used to constrain the effective temperatures of the components of young eclipsing double-lined spectroscopic binaries. Our method extends the approach of White et al. (1999) to a two-step analysis. The first step compares evolutionary models to the observed masses and radii and selects those models that predict ages that are consistent with coeval formation. The second step then uses these models to constrain the effective temperatures. We applied the method on literature values of the stellar parameters of the eclipsing binaries RX J0529.4+0041 A and V1174 Ori and confirm that V1174 Ori A has dwarf-like temperatures at an age of 9 Myrs, while we cannot draw any conclusions for RX J0529.4+0041 A and V1174 Ori B. Considering these binaries, we find that none of the evolutionary models gives coeval solutions simultaneously in mass, radius and effective temperature.