Brad M. S. Hansen et al. 2009 ApJ 691 382 doi:10.1088/0004-637X/691/1/382
Brad M. S. Hansen1, Hsin-Yi Shih1 and Thayne Currie1,2
Show affiliationsWe model the assembly of planets from planetary embryos under the conditions suggested by various scenarios for the formation of the planetary system around the millisecond pulsar B1257+12. We find that the most likely models fall at the low angular momentum end of the proposed range. Models that invoke supernova fallback produce such disks, although we find that a solar composition disk produces a more likely evolution than one composed primarily of heavy elements. Furthermore, we find that dust sedimentation must occur rapidly as the disk cools, in order that the solid material be confined to a sufficiently narrow range of radii. A quantitative comparison between the observations and the best-fit models shows that the simulations can reproduce the observed eccentricities and masses, but have difficulty reproducing the compactness of the pulsar planet system. Finally, we examine the results of similar studies of solar system terrestrial planet accumulation and discuss what can be learned from the comparison.
astrobiology; planetary systems: formation; pulsars: individual (PSR B1257+12); scattering
Issue 1 (2009 January 20)
Received 2008 July 9, accepted for publication 2008 September 22
Published 2009 January 14
Brad M. S. Hansen et al. 2009 ApJ 691 382
Ya Zhydachevskii et al 2006 J. Phys.: Condens. Matter 18 11385
Alexander Hubbard and Axel Brandenburg 2009 ApJ 706 712
Jun-Xian Wang et al. 2009 ApJ 706 762
Kenneth Miller et al. 2009 ApJ 690 720
Stijn Wuyts et al. 2009 ApJ 706 885
Michael C. Cushing et al. 2009 ApJ 706 923
Dean-Yi Chou et al. 2009 ApJ 706 909
E. D. Tenenbaum and L. M. Ziurys 2009 ApJ 694 L59
Jonathan T. Barron et al. 2008 The Astronomical Journal 135 414