2016A&A...586A.103W


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST01:25:46

2016A&A...586A.103W - Astronomy and Astrophysics, volume 586A, 103-103 (2016/2-1)

Consistent dust and gas models for protoplanetary disks. I. Disk shape, dust settling, opacities, and PAHs.

WOITKE P., MIN M., PINTE C., THI W.-F., KAMP I., RAB C., ANTHONIOZ F., ANTONELLINI S., BALDOVIN-SAAVEDRA C., CARMONA A., DOMINIK C., DIONATOS O., GREAVES J., GUEDEL M., ILEE J.D., LIEBHART A., MENARD F., RIGON L., WATERS L.B.F.M., ARESU G., MEIJERINK R. and SPAANS M.

Abstract (from CDS):

We propose a set of standard assumptions for the modelling of Class II and III protoplanetary disks, which includes detailed continuum radiative transfer, thermo-chemical modelling of gas and ice, and line radiative transfer from optical to cm wavelengths. The first paper of this series focuses on the assumptions about the shape of the disk, the dust opacities, dust settling, and polycyclic aromatic hydrocarbons (PAHs). In particular, we propose new standard dust opacities for disk models, we present a simplified treatment of PAHs in radiative equilibrium which is sufficient to reproduce the PAH emission features, and we suggest using a simple yet physically justified treatment of dust settling. We roughly adjust parameters to obtain a model that predicts continuum and line observations that resemble typical multi-wavelength continuum and line observations of ClassII TTauri stars. We systematically study the impact of each model parameter (disk mass, disk extension and shape, dust settling, dust size and opacity, gas/dust ratio, etc.) on all mainstream continuum and line observables, in particular on the SED, mm-slope, continuum visibilities, and emission lines including [OI]63µm, high-J CO lines, (sub-)mm CO isotopologue lines, and CO fundamental ro-vibrational lines. We find that evolved dust properties, i.e. large grains, often needed to fit the SED, have important consequences for disk chemistry and heating/cooling balance, leading to stronger near- to far-IR emission lines in general. Strong dust settling and missing disk flaring have similar effects on continuum observations, but opposite effects on far-IR gas emission lines. PAH molecules can efficiently shield the gas from stellar UV radiation because of their strong absorption and negligible scattering opacities in comparison to evolved dust. The observable millimetre-slope of the SED can become significantly more gentle in the case of cold disk midplanes, which we find regularly in our TTauri models. We propose to use line observations of robust chemical tracers of the gas, such as O, CO, and H2, as additional constraints to determine a number of key properties of the disks, such as disk shape and mass, opacities, and the dust/gas ratio, by simultaneously fitting continuum and line observations.

Abstract Copyright:

Journal keyword(s): stars: formation - circumstellar matter - radiative transfer - line: formation - astrochemistry - methods: numerical

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 V* FT Tau TT* 04 23 39.193 +24 56 14.11       14.37   M2.8 103 0
2 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1180 1
3 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 898 2
4 M 42 HII 05 35 17.3 -05 23 28           ~ 3657 0
5 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1442 1
6 THA 15-12 TT* 15 56 09.17658 -37 56 06.1193   10.7       M0e 214 0
7 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 10997 0
8 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 728 0

    Equat.    Gal    SGal    Ecl

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2019.10.17-01:25:46

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