TYC 2675-663-1: A newly discovered W UMa system in an active state

TL;DR

This study characterizes the newly discovered W UMa binary TYC 2675-663-1, revealing its overcontact nature, high mass ratio, and complex spectral features through extensive photometric and spectroscopic observations.

Contribution

It provides detailed photometric and spectroscopic analysis of TYC 2675-663-1, identifying it as a high mass ratio overcontact binary with potential third star influence.

Findings

Orbital period of 0.4223576 days.

Overcontact system with F5 and G7 stars.

Unusual spectral features including complex H alpha emission.

Abstract

The recently discovered eclipsing binary system TYC 2675-663-1 is a X-ray source, and shows properties in the optical that are similar to the W UMa systems, but are somewhat unusual compared to what is seen in other contact binary systems. The goal of this work is to characterize its properties and investigate its nature by means of detailed photometric and spectroscopic observations. We have performed extensive V-band photometric measurements with the INTEGRAL satellite along with ground-based multi-band photometric observations, as well as high-resolution spectroscopic monitoring from which we have measured the radial velocities of the components. These data have been analysed to determine the stellar properties, including the absolute masses and radii. Additional low-resolution spectroscopy was obtained to investigate spectral features. From the measured eclipse timings we determine an orbital period for the binary of P=0.4223576+-0.0000009 days. The light-curve and spectroscopic analyses reveal the observations to be well represented by a model of an overcontact system composed of main-sequence F5 and G7 stars (temperature difference of nearly 1000 K), with the possible presence of a third star. Low-resolution optical spectroscopy reveals a complex H alpha emission, and other features that are not yet understood. The unusually large mass ratio of q=0.81+-0.05 places it in the rare "H" (high mass ratio) subclass of the W UMa systems, which are presumably on their way to coalescence.