Abstract
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.
Highlights
Gas and dust disks are common objects; they can be observed around a variety of objects such as very young stars (e.g. T Tauri and Herbig Ae/Be stars), evolved binaries, and even black holes
We present a new code for the calculation of the 1D structure and synthetic spectra of accretion disks
We present a new 1D structure and radiative transfer program for circumstellar disks that is an extension of the general purpose stellar atmosphere code PHOENIX
Summary
Gas and dust disks are common objects; they can be observed around a variety of objects such as very young stars (e.g. T Tauri and Herbig Ae/Be stars), evolved binaries (cataclysmic variables), and even black holes. Meyer & Meyer-Hofmeister 1982; Cannizzo et al 1982) to obtain full numerical solutions for the structure of and the radiative transfer in accretion disks Since these models have reached a high degree of sophistication (for an overview of protoplanetary disk models see Dullemond et al 2007). High-resolution observations in combination with model spectra enable us to obtain kinematic information about the gas since line profiles are governed by the velocity field in the disk. Another interesting observation is the agreement of mean inner gas disk radii and orbital radii of shortperiod extrasolar planets (Carr 2007).
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