  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.
