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Planetesimal dynamics in self-gravitating protoplanetary discs

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Original languageEnglish
Title of host publicationMemorie della Società Astronomica Italiana
Publication statusPublished - 2005


The interaction between a gaseous protostellar disc and the embedded planetesimals through a drag force generally causes the latter to migrate inwards, the migration rate being very rapid (of the order of 103 yrs) for metre-size objects. Here we show how, in the presence of a spiral structure caused by the disc self-gravity, the drag force has the effect of concentrating significantly the planetesimals around the peaks of the gas density. Metre-size particles, in this configuration, can enhance their concentration by more than two orders of magnitude, therefore significantly accelerating their growth and the formation of the cores of giant planets.

    Research areas

  • accretion discs, stars: pre-main-sequence, planetary systems: formation planetary systems: protoplanetary discs

ID: 19690504