We model the assembly of planets from planetary embryos under the conditionssuggested by various scenarios for the formation of the planetary system aroundthe millisecond pulsar B1257+12. We find that the most likely models fall atthe low angular momentum end of the proposed range. Models that invokesupernova fallback produce such disks, although we find that a solarcomposition disk produces a more likely evolution than one composed primarilyof heavy elements. Furthermore, we find that dust sedimentation must occurrapidly as the disk cools, in order that the solid material be confined to asufficiently narrow range of radii. A quantitative comparison between theobservations and the best-fit models shows that the simulations can reproducethe observed eccentricities and masses, but have difficulty reproducing thecompactness of the pulsar planet system. Finally, we examine the results ofsimilar studies of solar system terrestrial planet accumulation and discusswhat can be learned from the comparison.
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