Issue |
A&A
Volume 632, December 2019
|
|
---|---|---|
Article Number | A44 | |
Number of page(s) | 28 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/201732187 | |
Published online | 29 November 2019 |
Radiation thermo-chemical models of protoplanetary disks
Grain and polycyclic aromatic hydrocarbon charging
1
Max Planck Institute for Extraterrestrial Physics,
Giessenbachstrasse,
85741
Garching,
Germany
2
Université Grenoble Alpes, CNRS, IPAG,
38000
Grenoble,
France
e-mail: geoffroy.lesur@univ-grenoble-alpes.fr
3
SUPA, School of Physics & Astronomy, University of St. Andrews,
North Haugh,
St. Andrews
KY16 9SS,
UK
4
Centre for Exoplanet Science, University of St Andrews,
St Andrews,
UK
5
Kapteyn Astronomical Institute,
PO Box 800,
9700 AV
Groningen,
The Netherlands
6
IRAP, Université de Toulouse, CNRS, UPS, CNES,
14 Avenue Edouard Belin,
Toulouse
31400,
France
Received:
27
October
2017
Accepted:
21
November
2018
Context. Disks around pre-main-sequence stars evolve over time by turbulent viscous spreading. The main contender to explain the strength of the turbulence is the magnetorotational instability model, whose efficiency depends on the disk ionization fraction.
Aims. Our aim is to compute self-consistently the chemistry including polycyclic aromatic hydrocarbon (PAH) charge chemistry, the grain charging, and an estimate of an effective value of the turbulence α parameter in order to find observational signatures of disk turbulence.
Methods. We introduced PAH and grain charging physics and their interplay with other gas-phase reactions in the physico-chemical code PRODIMO. Non-ideal magnetohydrodynamics effects such as ohmic and ambipolar diffusion are parametrized to derive an effective value for the turbulent parameter αeff. We explored the effects of turbulence heating and line broadening on CO isotopologue submillimeter lines.
Results. The spatial distribution of αeff depends on various unconstrained disk parameters such as the magnetic parameter βmag or the cosmic ray density distribution inside the protoplanetary disk s. The inner disk midplane shows the presence of the so-called dead zone where the turbulence is almost inexistent. The disk is heated mostly by thermal accommodation on dust grains in the dead zone, by viscous heating outside the dead zone up to a few hundred astronomical units, and by chemical heating in the outer disk. The CO rotational lines probe the warm molecular disk layers where the turbulence is at its maximum. However, the effect of turbulence on the CO line profiles is minimal and difficult to distinguish from the thermal broadening.
Conclusions. Viscous heating of the gas in the disk midplane outside the dead zone is efficient. The determination of α from CO rotational line observations alone is challenging.
Key words: astrochemistry / molecular data / stars: pre-main sequence / protoplanetary disks
© W. F. Thi et al. 2019
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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