  We show that Geminga's surface temperature can be understood by both types of
neutrino cooling scenarios, i.e, slow neutrino cooling by the modified Urca
process or fast neutrino cooling by the direct Urca process or by some exotic
matter, and thus does not allow us to discriminate between these two competing
schemes. However, for both types of scenarios, agreement with the observed
temperature can only be obtained if BARYON PAIRING IS PRESENT IN MOST, IF NOT
ALL, OF THE CORE OF THE STAR.
  We also comment on the recent temperature estimates for PSR 0656+14 and PSR
1055-52, which pertain to the same photon cooling era. We argue though that
observational evidence for the slow neutrino cooling model (the ``standard''
model) is in fact very dim and that the interpretation of the surface
temperature of all neutron stars could be done with a reasonable theoretical a
priori within the fast neutrino cooling scenarios only. In this case, Geminga,
PSR 0656+14, and PSR 1055-52 all show evidence of baryon pairing down to their
very centers. xxx----To be published in Ap.J. (June 10 isue).---xxx
