WAKELAM, Valentine; CHAPILLON, E.; DUTREY, Anne; GUILLOTEAU, S.; IQBAL, Wasim; COUTENS, Audrey; MAJUMDAR, A.

doi:10.1093/mnras/stz068

Métadonnées

Afficher la notice complète

Licence d’utilisation du document

WAKELAM, Valentine
AMOR 2019

CHAPILLON, E.
AMOR 2019

DUTREY, Anne
AMOR 2019

Langue

Article de revue

Ce document a été publié dans

Monthly Notices of the Royal Astronomical Society. 2019-01-09, vol. 484, n° 2, p. 1563-1573

Oxford University Press (OUP): Policy P - Oxford Open Option A

Résumé en anglais

Protoplanetary disks are challenging objects for astrochemical models due to strong density and temperature gradients and due to the UV photons 2D propagation. In this paper, we have studied the importance of several model parameters on the predicted column densities of observed species. We considered: 1) 2-phase (gas and homogeneous grains) or 3-phase (gas, surface, and bulk of grains) models, 2) several initial compositions, 3) grain growth and dust settling, and 4) several cosmic-ray ionization rates. Our main result is that dust settling is the most crucial parameter. Including this effect renders the computed column densities sensitive to all the other model parameters, except cosmic-ray ionization rate. In fact, we found almost no effect of this parameter for radii larger than 10 au (the minimum radius studied here) except for N2H+. We also compared all our models with all the column densities observed in the protoplanetary disk around DM Tau and were not able to reproduce all the observations despite the studied parameters. N2H+ seems to be the most sensitive species. Its observation in protoplanetary disks at large radius could indicate enough N2 in the gas-phase (inhibited by the 3-phase model, but boosted by the settling) and a low electron abundance (favored by low C and S elemental abundances).< Réduire

DOI

http://dx.doi.org/10.1093/mnras/stz068

Project ANR

Initiative d'excellence de l'Université de Bordeaux - ANR-10-IDEX-0003
FUTURE - ANR-16-IDEX-0003

Origine

Importé de hal

Unités de recherche

Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804