  Possessing the strongest magnetic fields in the Universe, magnetars mark an
extremum of physical phenomena. The strength of their magnetic fields is
sufficient to deform the shape of the stellar body, and when the rotational and
magnetic axes are not aligned, these deformations lead to the production of
gravitational waves (GWs) via a time-varying quadrupole moment. Such
gravitational radiation differs from signals presently detectable by the Laser
Interferometer Gravitational-Wave Observatory. These signals are continuous
rather than the momentary 'chirp' waveforms produced by binary systems during
the phases of inspiral, merger, and ringdown. We evaluate the sensitivity
requirements of future iterations of GW detectors to continuous GW signals
resulting from magnetars. Here, we construct a computational model for magnetar
stellar structure with strong internal magnetic fields. We implement an n = 1
polytropic equation of state (EOS) and adopt a mixed poloidal and toroidal
magnetic field model constrained by the choice of EOS. We utilize fiducial
values for magnetar magnetic field strength and various stellar physical
attributes. Via computational simulation, we measure the deformation of
magnetar stellar structure to determine upper bounds on the strength of
continuous GWs formed as a result of these deformations inducing
non-axisymmetric rotation. We compute predictions of upper limit GW strain
values for sources in the McGill Magnetar Catalog, an index of all detected
magnetars.
