Issue |
A&A
Volume 673, May 2023
|
|
---|---|---|
Article Number | A78 | |
Number of page(s) | 18 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202244767 | |
Published online | 10 May 2023 |
Toward a population synthesis of disks and planets
II. Confronting disk models and observations at the population level★
1
Universitäts-Sternwarte, Ludwig-Maximilians-Universität München,
Scheinerstraße 1,
81679
München, Germany
e-mail: emsenhuber@usm.lmu.de
2
Max-Planck-Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg, Germany
3
Physikalisches Institut, Universität Bern,
Gesellschaftsstrasse 6,
3012
Bern, Switzerland
4
Center for Astrophysics – Harvard & Smithsonian,
60 Garden Street,
Cambridge,
MA 02138,
USA
5
Excellence Cluster ‘Origins’,
Boltzmannstraße 2,
85748
Garching, Germany
Received:
18
August
2022
Accepted:
9
December
2022
Aims. We want to find the distribution of initial conditions that best reproduces disc observations at the population level.
Methods. We first ran a parameter study using a 1D model that includes the viscous evolution of a gas disc, dust, and pebbles, coupled with an emission model to compute the millimetre flux observable with ALMA. This was used to train a machine learning surrogate model that can compute the relevant quantity for comparison with observations in seconds. This surrogate model was used to perform parameter studies and synthetic disc populations.
Results. Performing a parameter study, we find that internal photoevaporation leads to a lower dependency of disc lifetime on stellar mass than external photoevaporation. This dependence should be investigated in the future. Performing population synthesis, we find that under the combined losses of internal and external photoevaporation, discs are too short lived.
Conclusions. To match observational constraints, future models of disc evolution need to include one or a combination of the following processes: infall of material to replenish the discs, shielding of the disc from internal photoevaporation due to magnetically driven disc winds, and extinction of external high-energy radiation. Nevertheless, disc properties in low-external-photoevaporation regions can be reproduced by having more massive and compact discs. Here, the optimum values of the α viscosity parameter lie between 3 × 10−4 and 10−3 and with internal photoevaporation being the main mode of disc dispersal.
Key words: protoplanetary disks / methods: numerical
Tables 3 and 4 are only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/673/A78
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://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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