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Pebble accretion onto planets in turbulent discs

Published online by Cambridge University Press:  13 January 2020

Wilhelm Kley Open the ORCID record for Wilhelm Kley [Opens in a new window] ,
Giovanni Picogna  and
Moritz H. R. Stoll
Wilhelm Kley
Affiliation:
Institut für Astronomie & Astrophysik, Universität Tübingen, Morgenstelle 10, D-72076 Tübingen, Germany email: wilhelm.kley@uni-tuebingen.de
Giovanni Picogna
Affiliation:
Universitätssternwarte, Universität München, Scheinerstr.1, D-81679 München, Germany email: picogna@usm.lmu.de
Moritz H. R. Stoll
Affiliation:
Institut für Astronomie & Astrophysik, Universität Tübingen, Morgenstelle 10, D-72076 Tübingen, Germany email: wilhelm.kley@uni-tuebingen.de
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Abstract

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Planets form in protoplanetary accretion discs around young protostars. These discs are driven by internal turbulence and the gas flow is not laminar but has stochastic components. For weakly ionised discs the turbulence can be generated purely hydrodynamically through the vertical shear instability (VSI). Embedded particles (dust/pebbles) experience a hydrodynamic drag and drift inward radially and are stirred up vertically by the turbulent motion of the disc. We study the accretion of particles onto a forming planet embedded in a VSI turbulent protoplanetary disc through a series of 3D hydrodynamical simulations for locally isothermal discs with embedded planets in the mass range from 5 to 100 Earth masses (M2295).

Keywords

hydrodynamicsplanetary systems: formationprotoplanetary disc
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. 237 - 238
Copyright
© International Astronomical Union 2020 

References

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Lambrechts, M. & Johansen, A., 2012, A&A, 572, A107 (LJ12)Google Scholar
Picogna, G., Stoll, M. H. R. & Kley, W., 2018, A&A, 616, A116 (PSK18)Google Scholar
Stoll, M.H.R. & Kley, W., 2016, A&A, 594, A57 (SK16)Google Scholar