Planetesimals drifting through dusty and gaseous white dwarf debris discs: Types I, II and III-like migration

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  • Dimitri Veras
    Centre for Exoplanets and Habitability, University of Warwick , Coventry CV4 7AL, UK
  • Shigeru Ida
    Earth-Life Science Institute, Tokyo Institute of Technology , Meguro, Tokyo 152-8550, Japan
  • Evgeni Grishin
    School of Physics and Astronomy, Monash University , Clayton, VIC 3800, Australia
  • Scott J Kenyon
    Smithsonian Astrophysical Observatory , 60 Garden Street, Cambridge, MA 02138, USA
  • Benjamin C Bromley
    Department of Physics and Astronomy, University of Utah , 201 JFB, Salt Lake City, UT 84112, USA

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<jats:title>ABSTRACT</jats:title> <jats:p>The suite of over 60 known planetary debris discs which orbit white dwarfs, along with detections of multiple minor planets in these systems, motivate investigations about the migration properties of planetesimals embedded within the discs. Here, we determine whether any of the migration regimes which are common in (pre-)main-sequence protoplanetary discs, debris discs, and ring systems could be active and important in white dwarf discs. We investigate both dust-dominated and gas-dominated regions, and quantitatively demonstrate that Type I and Type II migration, as well as their particulate disc analogues, are too slow to be relevant in white dwarf discs. However, we find that the analogue of Type III migration for particulate discs may be rapid in the dusty regions of asteroid- or moon-generated (&gt;1018 kg) white dwarf discs, where a planetesimal exterior to its Roche radius may migrate across the entire disc within its lifetime. This result holds over a wide range of disc boundaries, both within and exterior to 1R⊙, and such that the probability of migration occurring increases with higher disc masses.</jats:p>

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