  I describe models for the formation of planetary systems surrounding the
remnants of stellar mergers and collisions. I focus primarily on models for the
viscous evolution of disks suitable for the formation of the planets
surrounding the pulsar B1257+12. I show that the adaptation of models for
traditional protoplanetary disks which invoke quiescent or `dead' zones are
quite successful in producing disks appropriate for the formation of the pulsar
planets. I also briefly describe some even more exotic possibilities that may
arise from compact object mergers.
