  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.
