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3D radiation MHD simulations of gas and dust in protoplanetary disks

Published online by Cambridge University Press:  13 January 2020

Mario Flock Open the ORCID record for Mario Flock [Opens in a new window]
Mario Flock*
Affiliation:
Max-Planck Institut for Astronomy, Königstuhl 17, 69117, Heidelberg, Germany, email: [email protected]
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Abstract

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3D global radiation MHD simulations of gas and dust in protoplanetary disks allow us to understand the dynamical and thermal evolution of protoplanetary disks. At the same time, recent observations in the mm-dust emission by the Atacama Large Millimeter Array (ALMA) allow us to resolve structures at scales of the disk scale height.

From our recent simulation results by Flock et al. (2015) and Flock et al. (2017) we are able to directly compare for the first time detailed observational constraints from high-resolution observations by ALMA with the gas and dust dynamics obtain in 3D state-of-art simulations of protoplanetary disks. Especially measurements of the dust scale height obtained from the disk around the young system HL Tau allow us to compare for different gas disk instability models. Further we use Monte Carlo radiation transfer models of the dusty disk to compare our results of the dust scale height in 3D radiation HD and MHD simulations. Our findings are that magnetized models fit perfectly the observational constraints, showing a strongly settled disk, while hydrodynamical turbulence leads to a dust uplifting which is larger than expected. These results open a new window to compare future multi-wavelength observations to simulations.

Keywords

MHD simulationsaccretion disksprotoplanetary disksmm observations
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. 124 - 127
Copyright
© International Astronomical Union 2020 

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