  The interaction of an asteroid-mass primordial black hole (PBH) with a
slowly-rotating neutron star (NS) can lead to detectable gamma-ray emission via
modern observatories like Fermi-LAT or e-ASTROGRAM. Depending on the specific
PBH relativistic orbit in the NS Schwarschild spacetime and the relative
orientation of this binary system with respect to Earth, the PBH Hawking
radiation will show a characteristic temperature profile over time.
Essentially, a moderate heating behaviour (or even a progressive and constant
cooling phase) is found for the majority of the event, followed by a sudden and
dramatic cool-down at the end of the burst. Our theoretical model might provide
a means of identification of such hypothetical PBH-NS interactions, based on
the distinctive temperature evolution of thermal-like gamma ray bursts (GRBs)
described in this article.
