Physical parameters of W UMa type contact binaries and its stability of mass transfer

TL;DR

This paper analyzes the physical parameters and stability of mass transfer in W UMa contact binaries across different stellar mass ranges, classifying subclasses and examining their internal structure and evolution.

Contribution

It introduces a comprehensive dynamical model for W UMa binaries, exploring subclass distinctions and stability criteria using observational and theoretical parameters.

Findings

Determined physical parameters for A-, B-, and W-type W UMa systems.

Assessed stability using critical mass ratio and Roche lobe analysis.

Explored internal structure and evolution with polytropic models.

Abstract

In this study, we determined the physical parameters of W UMa type contact binaries and its stability of mass transfer with different stellar mass ranges over a broad space by applying the basic dynamical evolution equations of the W UMa type contact binaries using accretor and donor masses between 0.079 and 2.79 $M_{\odot}$. In these systems, we have studied the three sub-classes of the W UMa system such as A-, B- and W-type of W UMa contact binaries using the initial and final mass ranges and we investigated different stellar and orbital parameters for the sub-classes of W UMa systems. We examined the stability of the W UMa type contact binaries using the orbital parameters such as critical mass ratio, Roche lobe radius of the donor star, and mass ratio of these systems. Thus, we computed the observed and calculated physical parameters of A-, B- and W-type of W UMa systems. Although, we determined the combined and color temperatures to classify the three subclasses of the systems. Also, we have presented the result of the internal stellar structure and evolution of W UMa type contact binaries by using the polytropic model.