  We investigate the form of the radiation emitted by an axion star-neutron
star binary using a $f(r)=\text{sech(r/R)}$ profile for the axion star. Our
analysis takes into account the co-rotating plasma of the neutron star. We find
that that there is significant enhancement to the radiated power if the neutron
star's spin is tilted towards the plane of the axion star-neutron star orbit,
compared to the case where it is perpendicular. We also examine whether the
neutron star's co-rotating plasma can play a role in the emitted power and we
find that even though dilute axion stars can in principle radiate more
efficiently than dense axion stars, they will be pulled apart by the tidal
forces of the neutron star
