Stationary Population III accretion discs

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 occurrence 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, in both the structure and the stability behaviour. This is mainly owing to the absence of most molecules and dust in Pop III, which are very efficient absorbers in Pop I discs.