First photometric study of the eclipsing binary PS Persei

TL;DR

This study presents the first detailed photometric analysis of the eclipsing binary PS Persei, revealing its Algol-type nature, mass ratio, and orbital inclination, along with an improved orbital period estimate.

Contribution

It provides the first complete light curves analysis of PS Persei using the Wilson-Devinney code and refines its orbital period based on new and existing data.

Findings

PS Per is a short-period Algol-type binary.

The mass ratio is approximately 0.518.

The orbital inclination is nearly 89.86 degrees.

Abstract

The CCD photometric observations of the eclipsing binary PS Persei (PS Per) were obtained on two consecutive days in 2009. The 2003 version Wilson-Devinney code was used to analyze the first complete light curves in $V$ and $R$ bands. It is found that PS Per is a short-period Algol-type binary with the less massive component accurately filling its inner critical Roche lobe. The mass ratio of $q=0.518$ and the orbital inclination of $i=89.^{\circ}86$ are obtained. On the other hand, based on all available times of primary light minimum including two new ones, the orbital period has been improved.