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 |
|---|---|
| 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