Pebble formation by ice condensation
(2013) Workshop on Instabilities and Structures in Proto-Planetary Disks 46.- Abstract
- 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... (More)
- 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. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/3990536
- author
- Ros, Katrin LU
- organization
- publishing date
- 2013
- type
- Chapter in Book/Report/Conference proceeding
- publication status
- published
- subject
- host publication
- Instabilities And Structures In Proto-Planetary Disks
- volume
- 46
- publisher
- EDP Sciences
- conference name
- Workshop on Instabilities and Structures in Proto-Planetary Disks
- conference location
- Marseille, France
- conference dates
- 2012-09-17 - 2012-09-20
- external identifiers
-
- wos:000319936900026
- scopus:84876238165
- ISSN
- 2101-6275
- 2100-014X
- DOI
- 10.1051/epjconf/20134606005
- language
- English
- LU publication?
- yes
- id
- 969eee63-bcce-4bf4-9b28-ee0cb2b02a5a (old id 3990536)
- date added to LUP
- 2016-04-01 10:34:41
- date last changed
- 2024-01-06 20:09:11
@inproceedings{969eee63-bcce-4bf4-9b28-ee0cb2b02a5a,
abstract = {{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.}},
author = {{Ros, Katrin}},
booktitle = {{Instabilities And Structures In Proto-Planetary Disks}},
issn = {{2101-6275}},
language = {{eng}},
publisher = {{EDP Sciences}},
title = {{Pebble formation by ice condensation}},
url = {{http://dx.doi.org/10.1051/epjconf/20134606005}},
doi = {{10.1051/epjconf/20134606005}},
volume = {{46}},
year = {{2013}},
}