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Disk dynamics and planet migration

Abstract:

We review models of protoplanetary disks. In the earlier stages of evolution, disks are subject to gravitational instabilities that redistribute mass and angular momentum on short timescales. Later on, when the mass of the disk is below ten percent or so of that of the central star, accretion occurs through the magnetorotational instability. The parts of the disks that are not ionized enough to couple to the magnetic field may not accrete or accrete inefficiently. We also review theories of p...

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Publisher copy:
10.1051/eas/1041017

Authors


Terquem, CEJMLJ More by this author
Journal:
EAS Publications Series
Volume:
41
Pages:
209-218
Publication date:
2010
DOI:
EISSN:
1638-1963
ISSN:
1633-4760
URN:
uuid:2aaa4870-d0c3-4dc6-bcf6-51cb8f2aad44
Source identifiers:
389654
Local pid:
pubs:389654
Language:
English

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