the equilibrium configurations. Stationary toroidal configurations exist if $\ell\in (\ell_{\rm ms(i)},\ell_{\rm ms(o)})$. We can distinguish three kinds of discs (Fig. \[f3\]):

accretion discs:

:   $\ell\in (\ell_{\rm ms(i)},\ell_{\rm mb})$; the last closed surface is self-crossing in the inner cusp, another critical surface self-crossing in the outer cusp is open.

marginally bound accretion discs:

:   $\ell=\ell_{\rm mb}$; the last closed surface is self-crossing in both the inner and the outer cusp.

excretion discs:

:   $\ell\in (\ell_{\rm mb},\ell_{\rm ms(o)})$; the last closed surface is self-crossing in the outer cusp, another critical surface self-crossing in the inner cusp is open.

![Typical behaviour of equipotential surfaces (meridional sections) in the KdS black-hole spacetimes. Light gray region contains closed equipotential surfaces. The last closed surface is self-crossing in the cusp(s). Possible toroidal configurations correspond to: (a) accretion discs, (b) marginally bound accretion discs and (c) excretion discs.[]{data-label="f3"}](disk.eps){width="1\hsize"}

Conclusions
===========

For astrophysically relevant black holes ($M < 10^{12}M_{\odot}$) and the observed RRCC (\[E3\]), the cosmological parameter is so small ($y < 10^{-22}$) that both co-rotating and counter-rotating discs can exist around KdS black holes. The efficiency of the accretion process is then extremely close to the values relevant for Kerr black holes. The efficiency is strongest for 