The Absolute Parameters of The Detached Eclipsing Binary V482 Per

TL;DR

This study determines the absolute parameters of the detached eclipsing binary V482 Per, confirms orbital period variations likely caused by a third star, and analyzes the evolutionary states of its components.

Contribution

First to derive absolute parameters of V482 Per through combined photometric and spectroscopic analysis, and to suggest a third binary companion causing orbital period variations.

Findings

Absolute parameters of V482 Per derived for the first time.

Orbital period variations likely due to a third binary companion.

Primary slightly evolved post-Main Sequence, secondary still inside it.

Abstract

We present the results of the spectroscopic, photometric and orbital period variation analyses of the detached eclipsing binary \astrobj{V482~Per}. We derived the absolute parameters of the system (M$_{1}$ = 1.51 M$_{\odot}$, M$_{2}$ = 1.29 M$_{\odot}$, R$_{1}$ = 2.39 R$_{\odot}$, R$_{2}$ = 1.45 R$_{\odot}$, L$_{1}$ = 10.15 L$_{\odot}$, L$_{2}$ = 3.01 L$_{\odot}$) for the first time in literature, based on an analysis of our own photometric and spectroscopic observations. We confirm the nature of the variations observed in the system's orbital period, suggested to be periodic by earlier works. A light time effect due to a physically bound, star-sized companion (M$_{3}$ = 2.14 M$_{\odot}$) on a highly eccentric (e = 0.83) orbit, seems to be the most likely cause. We argue that the companion can not be a single star but another binary instead. We calculated the evolutionary states of the system's components, and we found that the primary is slightly evolving after the Main Sequence, while the less massive secondary lies well inside it.