Nature 353, 827 - 829 (31 October 1991); doi:10.1038/353827a0

Formation of a planet orbiting pulsar 1829–10 from the debris of a supernova explosion

D. N. C. Lin, S. E. Woosley & P. H. Bodenheimer

University of California Observatories/Lick Observatory, Board of Studies in Astronomy and Astrophysics, University of California, Santa Cruz, California 95064, USA

THE 10-Earth-mass planet¹ in a nearly circular 0.7-AU orbit around PSR1829–10 is unlikely to have survived the supernova, or especially the pre-supernova evolution of the star that became the pulsar. Here we describe how the planet might have been created inside the young supernova remnant^1–3. The principal difficulty lies not in providing enough mass or conducive thermo-dynamic conditions for planet formation, but in explaining the large angular momentum (3 x 10⁴⁸ erg s) and small eccentricity (<0.1) of the orbit. We propose that the planet formed from a rotationally supported disk of 0.02 solar mass of heavy elements that fell back from the supernova explosion to an initial radius of about 1,000 km. Viscous evolution of the disk then concentrated most of its angular momentum into a small amount of material at the disk's outer extremity: 10 Earth masses at 10¹³ cm. Here, dust grains that had condensed and precipitated towards the mid-plane grew through cohesive collisions and gravitational instabilities into 100-km planetesimals, which coagulated into the planet on a million-year timescale. We find the presence of a second planet, more massive and more distant, unlikely, although residual planetesimals may provide the fuel for -ray bursts.

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