General Relativistic Considerations of the Field Shedding Model of Fast
  Radio Bursts
  Popular models of fast radio bursts (FRBs) involve the gravitational collapse
of neutron star progenitors to black holes. It has been proposed that the
shedding of the strong neutron star magnetic field ($B$) during the collapse is
the power source for the radio emission. Previously, these models have utilized
the simplicity of the Schwarzschild metric which has the restriction that the
magnetic flux is magnetic "hair" that must be shed before final collapse. But,
neutron stars have angular momentum and charge and a fully relativistic Kerr
Newman solution exists in which $B$ has its source inside of the event horizon.
In this letter, we consider the magnetic flux to be shed as a consequence of
the electric discharge of a metastable collapsed state of a Kerr Newman black
hole. It has also been argued that the shedding model will not operate due to
pair creation. By considering the pulsar death line, we find that for a neutron
star with $B = 10^{11} - 10^{13}$ G and a long rotation period, $>1$ s this is
not a concern. We also discuss the observational evidence supporting the
plausibility of magnetic flux shedding models of FRBs that are spawned from
rapidly rotating progenitors.
