Radiative transfer in circumstellar disks - I. 1D models for GQ Lupi

TL;DR

This paper introduces a new 1D radiative transfer code for accretion disks, extending PHOENIX, capable of detailed spectral modeling including lines and dust, tested on GQ Lupi's protoplanetary disk spectra.

Contribution

The paper presents a novel 1D disk modeling code based on PHOENIX, incorporating extensive line lists and dust, specifically designed for analyzing protoplanetary disks.

Findings

Successfully modeled GQ Lupi's disk spectra with high resolution.

Demonstrated the code's capability to include molecular lines and dust.

Provided detailed disk structure and spectral predictions.

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.