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Gravitational fragmentation and formation of giant protoplanets on orbits of tens of AU

Published online by Cambridge University Press:  13 January 2020

Vardan G. Elbakyan Open the ORCID record for Vardan G. Elbakyan [Opens in a new window]  and
Eduard I. Vorobyov
Vardan G. Elbakyan
Affiliation:
Research Institute of Physics, Southern Federal University, Roston-on-Don, 344090Russia email: vgelbakyan@sfedu.ru
Eduard I. Vorobyov
Affiliation:
Research Institute of Physics, Southern Federal University, Roston-on-Don, 344090Russia email: vgelbakyan@sfedu.ru University of Vienna, Department of Astrophysics, Vienna, 1180, Austria email: eduard.vorobiev@univie.ac.at
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Abstract

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Migration of dense gaseous clumps that form in young protostellar disks via gravitational fragmentation is investigated to determine the likelihood of giant-planet formation. We show that gaseous clumps that form in the outer regions of the disk (> 100 au) through disk fragmentation often migrate toward the central star on timescales from a few thousand to few tens of thousands of years. The tidal mass loss helps the clumps to significantly slow down or even halt their inward migration at a distance of a few tens of AU from the protostar.

Keywords

stars: formationplanetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 234 - 236
Copyright
© International Astronomical Union 2020 

References

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