Statistical analysis of eclipsing binaries with monotonic orbital-period variations: A-type W UMa contact systems

TL;DR

This study analyzes monotonic orbital-period variations in A-type W UMa contact binaries to uncover relationships between binary parameters and mass transfer, mass loss, and angular momentum loss, revealing key correlations and power-law relationships.

Contribution

It introduces a method to link period variations with binary parameters and derives new power-law relationships, enhancing understanding of binary evolution mechanisms.

Findings

MT rate from primary to secondary depends on primary radius.

AML rate correlates with fill-out factor.

ML rate decreases with increasing mass ratio below ~0.46.

Abstract

On the basis of monotonic orbital-period variations, this study aims to identify genuine relationships between binary parameters and the rates of mass transfer (MT), mass loss (ML), and angular momentum loss (AML). Sample binaries with monotonic period variations are collected from the literature, together with well-determined binary parameters. Assuming the monotonic variations are responsible for any one of the MT, ML, and AML, their rates are calculated with the rates of change of period. After selecting crucial parameters using partial least-squares analysis, a parameter that exhibits the closest correlation with any one of the derived rates is further selected using partial regression plots. Moreover, power-law relationships are found for the discovered correlations. The properties of the sample binaries are also investigated by examining associations between binary parameters. In the systems with negative period variations, it is found that the rate of MT from more- to less-massive stars is a function of the primary radius; the AML rate is a function of the fill-out factor. In addition, the relationships between the mass ratio and stellar masses indicate that the ML rate relative to the MT rate decreases with increasing mass ratio below ~0.46. Meanwhile, in the systems with positive variations, it is found that the rate of MT from less- to more-massive stars is a function of the luminosity ratio and/or mass ratio; the ML rate is a function of the secondary temperature. The discussion also addresses possible processes occurring in the sample binaries.