2009/03/13 by S. D. Hügelmeyer, S. D. Huegelmeyer, S. Dreizler +4 · 8 citations
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Opacity #Planet #Radiative transfer #Scientific Research and Discoveries #Spectral line #Stellar atmosphere #T Tauri star #Thick disk #Thin disk #astro-ph.IM #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/200811536
published in Astronomy and Astrophysics 498(3), 793-800 (EDP Sciences) · 9 pages, 9 figures, accepted for publication in Astronomy & Astrophysics
arxiv created 2009/03/13 · openalex publication_date 2009/03/19 · arxiv updated 2015/05/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present a new code for the calculation of the 1D structure and synthetic spectra of accretion disks. The code is an extension of the general purpose stellar atmosphere code PHOENIX and is therefore capable of including extensive lists of atomic and molecular lines as well as dust in the calculations. We assume that the average viscosity can be represented by a critical Reynolds number in a geometrically thin disk and solve the structure and radiative transfer equations for a number of disk rings in the vertical direction. The combination of these rings provides the total disk structure and spectrum. Since the warm inner regions of protoplanetary disks show a rich molecular spectrum, they are well suited for a spectral analysis with our models. In this paper we test our code by comparing our models with high-resolution VLT CRIRES spectra of the T Tauri star GQ Lup.