The first photometric investigation and spectroscopic analysis of two contact binaries: ASAS J124343+1531.7 and LINEAR 2323566

TL;DR

This study presents the first photometric and spectroscopic analysis of two contact binaries, revealing their magnetic activity, orbital period changes, and evolutionary states through multi-telescope observations and data analysis.

Contribution

It provides the first detailed photometric and spectroscopic investigation of these two contact binaries, including their physical parameters and magnetic activity analysis.

Findings

ASAS J124343+1531.7 is a W-subtype median contact binary.

LINEAR 2323566 is a W-subtype shallow contact binary.

Both systems exhibit magnetic activity and O'Connell effect.

Abstract

The multi-color passband CCD light curves of ASAS J124343+1531.7 and LINEAR 2323566 were first obtained by the 0.84-m Ritchey-Chr\'{e}tien telescope with follow up observations by the WIYN 0.90m Cassegrain telescope. The data from the $Transiting\quad Exoplanet\quad Survey\quad Satellite\quad (TESS)$ of ASAS J124343+1531.7 was also applied for subsequent analysis. By analyzing the data through the W-D program, their mass ratios and fill-out factors were determined as 3.758, 1.438 and 31.8$\%$, 14.9$\%$, respectively. ASAS J124343+1531.7 is a W-subtype median contact binary, while LINEAR 2323566 is a W-subtype shallow contact binary, and the asymmetric light curves prove that they both have the O'Connell effect, which is generally explained by magnetic activity. The equivalent widths (EWs) of H$_\alpha$ lines were calculated, which show they certainly have magnetic activity. Moreover, LINEAR 2323566 has a stronger magnetic activity. The analysis of orbital period changes shows that ASAS J124343+1531.7 has a trend of secular period increase, which is generally explained by the mass transfer from the less massive to the more massive star. According to the estimated absolute parameters, their evolutionary states are discussed. The two components of ASAS J124343+1531.7 are both main sequence stars. While for LINEAR 2323566, the more massive star is a main sequence star, the less massive star has evolved out of main sequence and is over-luminous and over-sized.