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Retention of Small Charged Dust in Planet Forming Disks

Published online by Cambridge University Press:  13 January 2020

Vitaly Akimkin Open the ORCID record for Vitaly Akimkin [Opens in a new window]
Vitaly Akimkin*
Affiliation:
Institute of Astronomy, Russian Academy of Sciences 119017, Pyatnitskaya str. 48, Moscow, Russia email: akimkin@inasan.ru
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Abstract

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Dust evolution in disks around young stars is a key ingredient for the global disk evolution and accompanying planet formation. The mutual sticking of initially small grains is not straightforward and can be hampered by several processes. This includes dust grain bouncing, fragmentation, electrostatic repulsion and fast drift to the central star. In this study we aim at theoretical modeling of the dust coagulation coupled with the dust charging and disk ionization calculations. We show that the electrostatic barrier is a strong restraining factor to the coagulation of micron-size dust. While the sustained turbulence helps to overcome the electrostatic barrier, dust fluffiness limits this opportunity. Coulomb repulsion may keep a significant fraction of m dust in large regions of protoplanetary disks.

Keywords

accretionaccretion disksplasmasturbulencedustextinctioncosmic rays
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. 283 - 284
Copyright
© International Astronomical Union 2020 

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