2D disc modelling of the JWST line spectrum of EXLupi

P. Woitke*, W. F. Thi, A. M. Arabhavi, I. Kamp, A. Kóspál, P. Ábrahám

*Corresponding author for this work

Research output: Contribution to journalArticleAcademicpeer-review

2 Citations (Scopus)
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Abstract

We introduce a number of improvements to the thermo-chemical disc modelling code ProDiMo and new theoretical approaches that can be used to better predict and analyse the JWST line spectra of protoplanetary discs. We developed a new line escape probability method for disc geometries, and a new scheme for dust settling, and discuss how to apply UV molecular shielding factors to photo rates in 2D disc geometry. We show that these assumptions are crucial for the determination of gas heating and cooling rates and discuss how they affect the predicted molecular concentrations and line emissions. We apply our revised 2D models to the protoplanetary disc around the T Tauri star EXLupi in quiescent state. We calculate infrared line emission spectra between 5 and 20 μm from CO, H2O, OH, CO2, HCN, C2H2, and H2, including lines of atoms and ions, using our full 2D predictions of molecular abundances, dust opacities, and gas and dust temperatures. We developed a disc model with a slowly increasing surface density structure around the inner rim that can simultaneously fit the spectral energy distribution, the overall shape of the JWST spectrum of EXLupi, and the main observed molecular characteristics in terms of column densities, emitting areas, and molecular emission temperatures, which all result from one consistent disc model. The spatial structure of the line-emitting regions of the different molecules is discussed. High abundances of HCN and C2H2 are caused in the model by stellar X-ray irradiation of the gas around the inner rim.

Original languageEnglish
Article numberA219
Number of pages28
JournalAstronomy and Astrophysics
Volume683
DOIs
Publication statusPublished - 1-Mar-2024

Keywords

  • astrochemistry
  • line: formation
  • methods: numerical
  • protoplanetary disks

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