  Non-thermal correction to the emission probability of particles from black
holes can be obtained if the backreaction or self-gravitational effects of the
emitted particles on the black hole spacetime are taken into consideration.
These non-thermally emitted particles conserve the entropy of the black hole,
i.e, the entropy of the system of radiated particles after complete evaporation
of the black hole matches the initial entropy of the black hole. Using the
non-thermal emission probability, we have determined the probability for a
black hole of mass $M$ to be completely evaporated by a given number of
particles $n$. This is done by first evaluating the number of possible ways in
which the black hole can be evaporated by emitting $n$ number of particles, and
then the total number of ways in which the black hole can be evaporated. The
ratio of these two quantities gives us the desired probability. From the
probability distribution, we get a displacement relation between the most
probable number of particles exhausting the black hole and the temperature of
the initial black hole. This relation resembles Wien's displacement law for
blackbody radiation.
