Far-ultraviolet and X-ray irradiated protoplanetary disks: a grid of models. II. Gas diagnostic line emission - INSU - Institut national des sciences de l'Univers Access content directly
Journal Articles Astronomy and Astrophysics - A&A Year : 2012

Far-ultraviolet and X-ray irradiated protoplanetary disks: a grid of models. II. Gas diagnostic line emission

G. Aresu
  • Function : Author
R. Meijerink
  • Function : Author
I. Kamp
  • Function : Author
M. Spaans
  • Function : Author
P. Woitke
  • Function : Author

Abstract

Context. Most of the mass in protoplanetary disks is in the form of gas. The study of the gas and its diagnostics is of fundamental importance in order to achieve a detailed description of the thermal and chemical structure of the disk. Both radiation from the central star (from optical to X-ray wavelengths) and viscous accretion are the main sources of energy, dominating disk physics and chemistry in its early stages. This is the environment in which the first phases of planet formation will proceed.
Aims: We investigate how stellar and disk parameters impact the fine-structure cooling lines [Ne ii], [Ar ii], [O i], [C ii], and H2O rotational lines in the disk. These lines are potentially powerful diagnostics of the disk structure, and their modeling permits a thorough interpretation of the observations carried out with instrumental facilities such as Spitzer and Herschel.
Methods: Following our earlier paper, we computed a grid of 240 disk models, in which the X-ray luminosity, UV-excess luminosity, minimum dust grain size, dust size distribution power law, and surface density distribution power law are systematically varied. We solve self-consistently for the disk vertical hydrostatic structure in every model and apply detailed line radiative transfer to calculate line fluxes and profiles for a series of well-known mid- and far-infrared cooling lines.
Results: The [O i] 63 μm line flux increases with increasing LFUV when LX < 1030 erg s-1 and with increasing X-ray luminosity when LX > 1030 erg s-1. While [C ii] 157 μm is mainly driven by LFUV via C+ production, X-rays affect the line flux to a lesser extent. In addition, [Ne ii] 12.8 μm correlates with X-rays; the line profile emitted from the disk atmosphere shows a double-peaked component caused by emission in the static disk atmosphere, next to a high-velocity double-peaked component caused by emission in the very inner rim. Water transitions, depending on the disk region they arise from, show different slopes in correlation with the [O i] 63 μm line.
Fichier principal
Vignette du fichier
aa19864-12.pdf (1.85 Mo) Télécharger le fichier
Origin Publisher files allowed on an open archive

Dates and versions

insu-03612397 , version 1 (17-03-2022)

Licence

Identifiers

Cite

G. Aresu, R. Meijerink, I. Kamp, M. Spaans, W. -F. Thi, et al.. Far-ultraviolet and X-ray irradiated protoplanetary disks: a grid of models. II. Gas diagnostic line emission. Astronomy and Astrophysics - A&A, 2012, 547, ⟨10.1051/0004-6361/201219864⟩. ⟨insu-03612397⟩
40 View
13 Download

Altmetric

Share

Gmail Mastodon Facebook X LinkedIn More