Examining the brightness variability, accretion disk, and evolutionary stage of the binary OGLE-LMC-ECL-14413

TL;DR

This study investigates the brightness variability, accretion disk dynamics, and evolutionary status of the binary system OGLE-LMC-ECL-14413 over 30 years, revealing complex disk behavior and system parameters through detailed modeling and simulations.

Contribution

It provides the first comprehensive analysis of the long-term brightness variations and accretion disk structure in OGLE-LMC-ECL-14413, combining observational data with stellar evolution modeling.

Findings

Orbital period of 38.15917 days identified.

Long-term cycle of approximately 780 days observed.

Disk contains variable properties with shock regions.

Abstract

Our study aims to elucidate both short-term and long-term variations in the light curve of the eclipsing system OGLE-LMC-ECL-14413, with a particular focus on the unusual reversals in eclipse depth. We aim to clarify the role of the accretion disk in these fluctuations, especially in long-cycle changes spanning hundreds of days. Additionally, we seek to determine the evolutionary stage of the system and gain insights into the internal structure of its stellar components. We analyzed photometric time series from the Optical Gravitational Lensing Experiment (OGLE) project in the I and V bands, and from the MAssive Compact Halo Objects project in the BM and RM bands, covering a period of 30.85 years. Using light curve data from 27 epochs, we constructed models of the accretion disk. An optimized simplex algorithm was employed to solve the inverse problem, deriving the best-fit parameters for the stars, orbit, and disk. We also utilized the Modules for Experiments in Stellar Astrophysics software to assess the evolutionary stage of the binary system, investigating the progenitors and potential future developments. We found an orbital period of 38.15917(54) d and a long-term cycle of approximately 780 d. Temperature, mass, radius, and surface gravity values were determined for both stars. The photometric orbital cycle and the long-term cycle are consistent with a disk containing variable physical properties, including two shock regions. The disk encircles the more massive star and the system brightness variations align with the long-term cycle at orbital phase 0.25. Our mass transfer rate calculations correspond to these brightness changes. \texttt{MESA} simulations indicate weak magnetic fields in the donor star's subsurface, which are insufficient to influence mass transfer rates significantly.