  We further investigate the runaway instability of relativistic tori around
black holes assuming a power law distribution of the specific angular momentum.
We neglect the self-gravity of the torus; thus the gravitational field of the
system is determined by the central rotating black hole alone (the Kerr
geometry). We find that for any positive (i.e. consistent with the local
Rayleigh stability condition) power law index of the angular momentum
distribution, the tori are always runaway stable for a sufficiently large spin
of the black hole. However, before concluding that some (astrophysically
realistic) tori could indeed be runaway stable, one should include, in full
general relativity, the destabilizing effect of self-gravity.
