Circumpulsar disk evolution and pulsar planet formation
          Thayne Currie, UCLA
          Brad Hansen, UCLA

          We investigate the evolution of a viscous protoplanetary disk around a millisecond pulsar where a tidally disrupted pre-supernova companion is assumed to be the source for disk mass.  Calculations for the temperature and surface density profile are contrasted for various fully viscous disk models and 'layered disk' models for a range of initial angular momentum values J = 10^51 - 10^53 ergs s, corresponding to a range of initial companion masses of ~ 0.01-1 solar masses.  We further examine the planetary system of PSR 1257+12 in light of these calculations and contrast the existing architecture of that system with expectations for the masses and semimajor axes of planets from this disk modeling.