Stationary Population III accretion discs
Abstract
We present stationary models of protostellar population III (Pop III, for short) accretion discs, compare them to Pop I discs, and investigate the influence of the different chemical compositions on the occurence of gravitational, thermal and thermal-viscous instabilities in the discs. In particular in the cooler regions, we find major differences between Pop III and Pop I discs, both in the structure and stability behaviour. This is mainly due to the absence of most molecules and dust in Pop III, which are very efficient absorbers in Pop I discs.
Keywords
Cite
@article{arxiv.astro-ph/0406501,
title = {Stationary Population III accretion discs},
author = {Michael Mayer and Wolfgang J. Duschl},
journal= {arXiv preprint arXiv:astro-ph/0406501},
year = {2009}
}
Comments
12 pages, 6 figures, resubmitted to MNRAS, very minor changes made in response to latest referee report, Figure 1+2 only in low-res, for high-res colour PDF file see http://www.ita.uni-heidelberg.de/~mm/publications/MayerDuschl-1.pdf