  In this work, we develop a perturbative method to describe the behavior of a
chiral condensate around a spherical black hole whose mass is astrophysically
realistic. We use the inverse mass as the expansion parameter for our
perturbative series. We test this perturbative method in the case of a
Schwarzschild black hole, and we find that it agrees well with previous
numerical results. For an astrophysical-mass Schwarzschild black hole, the
leading order contribution to the condensate is much larger (in most of space)
than the next-to-leading order contribution, providing further evidence for the
validity of the perturbative approach. The size of the bubble of restored
chiral symmetry is directly proportional to the size of the black hole. Next,
we apply this perturbative method to a Reissner-Nordstr\"om (RN) black hole. We
find that, as the charge-to-mass ratio increases, the bubble of restored chiral
symmetry becomes larger relative to the black hole. This effect is particularly
pronounced for near-extremal RN black holes. The case of an extremal RN black
hole provides an interesting counterexample to the standard thermal explanation
for the formation of a bubble of restored chiral symmetry around a black hole.
