# Fundamental properties of the pre-main sequence eclipsing stars of MML 53 and the mass of the tertiary

## TL;DR

This study provides a detailed analysis of the MML 53 eclipsing binary system, confirming the third star's bound nature, measuring stellar parameters with high precision, and discussing implications for early binary formation and stellar evolution models.

## Contribution

First comprehensive analysis of MML 53, including the third star, with precise measurements of stellar masses, radii, and temperature, and insights into early binary formation mechanisms.

## Key findings

- Masses measured within 1% accuracy
- Radii inflated by 10-20% compared to models
- Third star's mass confirmed around 0.7 Msun

## Abstract

We present the most comprehensive analysis to date of the Upper Centaurus Lupus eclipsing binary MML 53 (2.097892 d), and for the first time, confirm the bound-nature of the third star (~9yr orbit). Our analysis uses new and archival spectra and time-series photometry. We determined the temperature of the primary star to be 4880+-100 K. The study of the close binary incorporated treatment of spots and dilution by the tertiary in the light curves, allowing for the robust measurement of the masses of the eclipsing components within 1% (M1=1.0400+-0.0067 and M2=0.8907+-0.0058 Msun), their radii within 4.5% (R1=1.283+-0.043 and R2=1.107+-0.049 Rsun), and the secondary temperature (4379+-100K). From the analysis of the eclipse timings, and the change in systemic velocity of the eclipsing binary and the radial velocities of the third star, we measured the mass of the outer companion to be 0.7 Msun within 20%. The age we derived from the evolution of the temperature ratio between the eclipsing components is fully consistent with previous estimates of the age of UCL (16+-2 Myr). At this age, the tightening of the MML 53 eclipsing binary has already occurred, thus supporting close-binary formation mechanisms that act early in their evolution. The eclipsing stars roughly follow the same theoretical isochrone, but appear to be inflated in radius (by 20% for the primary and 10% for the secondary). However, our primary radius measurement of is in full agreement with the independent measurement of the secondary of NP Per which has the same mass and a similar age. The eclipsing stars of MML 53 are found to be larger but not cooler than predicted by non-magnetic models, it is not clear what is the mechanism that is causing the radius inflation given that activity, spots and/or magnetic fields slowing their contraction, require the inflated stars to be cooler to remain in thermal equilibrium.