Circumpulsar disk evolution and pulsar planet formation
Authors:
Thayne Currie,
UCLA
Brad Hansen, UCLA
Abstract:
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.