Abstract
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.
Original language | English |
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Title of host publication | Memorie della Società Astronomica Italiana |
Pages | 325 |
Volume | 76 |
Publication status | Published - 2005 |
Keywords / Materials (for Non-textual outputs)
- accretion discs
- stars: pre-main-sequence
- planetary systems: formation planetary systems: protoplanetary discs