  We show that the magnetic dipole and gravitational radiation emitted by a
pulsar can undergo superradiant scattering off a spinning black hole companion.
We find that the relative amount of superradiant modes in the radiation depends
on the pulsar's angular position relative to the black hole's equatorial plane.
In particular, when the pulsar and black hole spins are aligned, superradiant
modes are dominant at large angles, leading to an amplification of the pulsar's
luminosity, whereas for small angles the radiation is dominantly composed of
non-superradiant modes and the signal is attenuated. This results in a
characteristic orbital modulation of the pulsar's luminosity, up to the percent
level within our approximations, which may potentially yield a signature of
superradiant scattering in astrophysical black holes and hence an important
test of general relativity.
