Properties of white dwarf in the binary system AR Scorpii and its observed features

TL;DR

This paper investigates the physical properties and observed features of the white dwarf in the AR Scorpii binary system, exploring its emission mechanisms, magnetic field effects, and gravitational wave potential.

Contribution

It provides a detailed analysis of the white dwarf's properties and their connection to observed emissions, offering new insights into the system's behavior.

Findings

White dwarf's magnetic field influences accretion activity.

Spin-down power correlates with broadband emission features.

Potential gravitational wave emission due to magnetic deformation.

Abstract

The binary system AR Scorpii hosts an M-type main sequence cool star orbiting around a magnetic white dwarf in the Milky Way Galaxy. The broadband non-thermal emission over radio, optical and X-ray wavebands observed from AR Scorpii indicates strong modulations on the spin frequency of the white dwarf as well as the spin-orbit beat frequency of the system. Therefore, AR Scorpii is also referred to as a white dwarf pulsar wherein a fast spinning white dwarf star plays very crucial role in the broadband non-thermal emission. Several interpretations for the observed features of AR Scorpii appear in the literature without firm conclusions. In this work, we investigate connection between some of the important physical properties like spin-down power, surface magnetic field, equation of state, temperature and gravity associated with the white dwarf in the binary system AR Scorpii and its observational characteristics. We explore the plausible effects of white dwarf surface magentic field on the absence of substantial accretion in this binary system and also discuss the gravitational wave emission due to magnetic deformation mechanism.