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The gas structure of the HD 163296 planet-forming disk - gas gaps or not?

Published online by Cambridge University Press:  12 October 2020

C. Rab Open the ORCID record for C. Rab [Opens in a new window] ,
G. A. Muro-Arena ,
I. Kamp Open the ORCID record for I. Kamp [Opens in a new window] ,
C. Dominik ,
L. B. F. M. Waters ,
W-F. Thi  and
P. Woitke
C. Rab
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, the Netherlands email: rab@astro.rug.nl
G. A. Muro-Arena
Affiliation:
Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
I. Kamp
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, the Netherlands email: rab@astro.rug.nl
C. Dominik
Affiliation:
Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands
L. B. F. M. Waters
Affiliation:
Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, the Netherlands SRON Netherlands, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands
W-F. Thi
Affiliation:
MPE, Giessenbachstrasse 1, 85748 Garching, Germany
P. Woitke
Affiliation:
SUPA, School of Physics & Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK
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Abstract

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HD 163296 is a young star surrounded by a planet-forming disk that shows clear signatures of dust gaps and rings; likely an indication of ongoing planet formation. We use the radiation thermochemical disk code ProDiMo to investigate the impact of dust/gas gaps on the temperature, chemistry and observables. Furthermore, we model high spatial resolution gas and dust observation of HD 163296 (ALMA/DSHARP). Our first results indicate that features in the observed radial intensity profile of the 12CO line are a consequence of the dust gaps and do not require gas depletion. Those preliminary results indicate that self-consistent modelling of the gas (chemistry, heating/cooling) and dust is necessary to accurately infer the degree of gas depletion within dust gaps. Such information is crucial to understand the processes that generate the disk substructure and their relation to planet formation.

Keywords

stars: pre–main-sequence(stars:) planetary systems: protoplanetary disksastrochemistryradiative transfermethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 445 - 447
Copyright
© International Astronomical Union 2020

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