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Modeling protoplanetary disk evolution in young star forming regions

Published online by Cambridge University Press:  20 January 2023

Martijn J. C. Wilhelm Open the ORCID record for Martijn J. C. Wilhelm [Opens in a new window] ,
Simon Portegies Zwart ,
Claude Cournoyer-Cloutier ,
Sean Lewis ,
Brooke Polak ,
Aaron Tran ,
Mordecai-Mark Mac Low  and
Stephen L. W. McMillan
Martijn J. C. Wilhelm
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA, Leiden, the Netherlands email: wilhelm@strw.leidenuniv.nl
Simon Portegies Zwart
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA, Leiden, the Netherlands email: wilhelm@strw.leidenuniv.nl
Claude Cournoyer-Cloutier
Affiliation:
Department of Physics and Astronomy, McMaster University, Hamilton, Canada
Sean Lewis
Affiliation:
Department of Physics, Drexel University, Philadelphia, USA
Brooke Polak
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie, Universität Heidelberg, Heidelberg, Germany
Aaron Tran
Affiliation:
Department of Astronomy, Columbia University, New York, USA
Mordecai-Mark Mac Low
Affiliation:
Department of Astronomy, Columbia University, New York, USA Department of Astrophysics, American Museum of Natural History, New York, USA
Stephen L. W. McMillan
Affiliation:
Department of Physics, Drexel University, Philadelphia, USA
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Abstract

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Stars form in clusters, while planets form in gaseous disks around young stars. Cluster dissolution occurs on longer time scales than disk dispersal. Planet formation thus typically takes place while the host star is still inside the cluster. We explore how the presence of other stars affects the evolution of circumstellar disks. Our numerical approach requires multi-scale and multi-physics simulations where the relevant components and their interactions are resolved. The simulations start with the collapse of a turbulent cloud, from which stars with disks form, which are able to influence each other. We focus on the effect of extinction due to residual cloud gas on the early evolution of circumstellar disks. We find that this extinction protects circumstellar disks against external photoevaporation, but these disks then become vulnerable to dynamic truncation by passing stars. We conclude that circumstellar disk evolution is heavily affected by the early evolution of the cluster.

Keywords

methods: numericalstars: formationplanetary systems: protoplanetary disksISM: clouds
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 300 - 305
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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