The Evolution of Protoplanetary Disks Around Millisecond Pulsars: The PSR 1257 +12 System
Abstract
We model the evolution of protoplanetary disks surrounding millisecond pulsars, using PSR 1257+12 as a test case. Initial conditions were chosen to correspond to initial angular momenta expected for supernova-fallback disks and disks formed from the tidal disruption of a companion star. Models were run under two models for the viscous evolution of disks: fully viscous and layered accretion disk models. Supernova-fallback disks result in a distribution of solids confined to within 1-2 AU and produce the requisite material to form the three known planets surrounding PSR 1257+12. Tidal disruption disks tend to slightly underproduce solids interior to 1 AU, required for forming the pulsar planets, while overproducing the amount of solids where no body, lunar mass or greater, exists. Disks evolving under 'layered' accretion spread somewhat less and deposit a higher column density of solids into the disk. In all cases, circumpulsar gas dissipates on year timescales, making formation of gas giant planets highly unlikely.
Keywords
Cite
@article{arxiv.0705.3063,
title = {The Evolution of Protoplanetary Disks Around Millisecond Pulsars: The PSR 1257 +12 System},
author = {Thayne Currie and Brad Hansen},
journal= {arXiv preprint arXiv:0705.3063},
year = {2019}
}
Comments
16 pages, 17 figures, Accepted for publication in The Astrophysical Journal (September 20, 2007 issue)