  Hiscock and Weems showed that under Hawking evaporation, an isolated
asymptotically flat Reissner-Nordstrom (RN) black hole evolves in a surprising
manner: if it starts with a relatively small value of charge-to-mass ratio Q/M,
then said value will temporarily increase along its evolutionary path, before
finally decreases towards zero. This contrasts with highly charged ones that
simply radiate away its charge steadily. The combination of these two effects
is the cosmic censor at work: there exists an attractor that flows towards the
Schwazschild limit, which ensures that extremality -- and hence naked
singularity -- can never be reached under Hawking evaporation. We apply the
scheme of Hiscock and Weems to model the evaporation of an asymptotically flat
dilatonic charge black hole known as the Garfinkle-Horowitz-Strominger (GHS)
black hole. We found that upholding the cosmic censorship requires us to modify
the charged particle production rate, which remarkably agrees with the
expression obtained independently via direct computation of charged particle
production rate on curved spacetime background. This not only strengthens the
case for cosmic censorship, but also provides an example in which cosmic
censorship can be a useful principle to deduce other physics. We also found
that the attractor behavior is not necessarily related to the specific heat,
contrary to the claim by Hiscock and Weems.
