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Evolution of solids in planet forming disks: The interplay of experiments, simulations, and observations

Published online by Cambridge University Press:  12 October 2020

T. Birnstiel Open the ORCID record for T. Birnstiel [Opens in a new window]
T. Birnstiel*
Affiliation:
University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany email: til.birnstiel@lmu.de
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Abstract

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Circumstellar dust analogues can be studied experimentally to determine their collisional behavior and their optical properties. These results affect simulations of circumstellar disks in various, substantial ways: Collision results determine how dust aggregates grow and how their aerodynamic properties change with time. This determines how solids move throughout the disk, how they accumulate, and how planetesimals might be formed. The optical properties determine the observational signature of these effects and allow us to constrain the spatial distribution of dust in disks, the sizes of the aggregates, as well as the temperature and optical depth of the dust emission. In this contribution, it is discussed how theoretical models and their predictions depend on laboratory results and what we learned about disks from high spatial resolution radio interferometry.

Keywords

planetary systems: protoplanetary diskscircumstellar matterscatteringsubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 200 - 204
Copyright
© International Astronomical Union 2020

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