  In view of the new recent observation and measurement of the rotating and
highly-magnetized white dwarf AR Scorpii \cite{Marsh:2016uhc}, we determine
bounds of its moment of inertia, magnetic fields and radius. Moreover, we
investigate the possibility of fast rotating and/or magnetized white dwarfs to
be source of detectable gravitational wave (GW) emission. Numerical stellar
models at different baryon masses are constructed. For each star configuration,
we compute self-consistent relativistic solutions for white dwarfs endowed with
poloidal magnetic fields by solving the Einstein-Maxwell field equations in a
self-consistent way. The magnetic field supplies an anisotropic pressure,
leading to the braking of the spherical symmetry of the star. In this case, we
compute the quadrupole moment of the mass distribution. Next, we perform an
estimate of the GW of such objects. Finally, we show that the new recent
observation and measurement pulsar white dwarf AR Scorpii, as well other
stellar models, are able to generate gravitational wave radiation that lies in
the bandwidth of the discussed next generation of space-based GW detectors
DECI-hertz interferometer Gravitational wave Observatory (DECIGO) and Big Bang
Observer (BBO).
