EPJ Web of Conferences
Volume 46, 2013Instabilities and Structures in Proto-Planetary Disks
|Number of page(s)||4|
|Section||Capture and Dust Loading|
|Published online||11 April 2013|
Pebble formation by ice condensation
Lund Observatory, Department of Astronomy and
Theoretical Physics, Lund University, Box 43, 221 00
a e-mail: firstname.lastname@example.org
Pebbles with sizes of centimeters to decimeters are needed in order to form kilometer-sized planetesimals, which in turn are needed for planet formation to proceed. The well-studied mechanism of coagulation is efficient only up to millimeter-sized dust grains. In this proceeding a numerical model of ice condensation as a complementary growth mechanism in turbulent protoplanetary discs is discussed. Close to an ice line, particles grow efficiently by ice condensation, which, combined with radial mixing, can supply a large extent of the disc with icy pebbles. Growth from millimeter-sized dust grains to at least decimeter-sized pebbles is possible on a time scale of only 10 000 years. The resulting particles are large enough to enable further growth into planetesimals via a variety of particle concentration mechanisms and subsequent gravitational collapse.
© Owned by the authors, published by EDP Sciences, 2013
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