thin, Keplerian discs orbiting extreme black holes. It is suppressed for $a$ descending and/or for $\ell = \mbox{const}$ growing from $\ell_{\rm ms(i)}$ up to $\ell_{\rm mb}$. Notice that the co-rotating toroidal discs are steeper and more extended than the counter-rotating discs.

The crucial effects caused by the RRCC are illustrated in (Fig. \[f4\]).

-   The outer edge of the discs. The presence of an outer cusp of toroidal discs nearby the static radius enables outflow of mass and angular momentum from the discs due to a violation of mechanical equilibrium. Recall that such an outflow is impossible from discs around isolated black holes in asymptotically flat spacetimes.[@Koz-Jar-Abr:1978:ASTRA:]

-   Strong collimation effect on jets escaping along the rotational axis of toroidal discs indicated by open equipotential surfaces that are narrowing strongly after crossing the static radius.

![Shapes of thick discs and collimation of jets due to a cosmic repulsion. The effect of collimation is relevant near the static radius and further. Left picture depicts thick accretion discs orbiting the Kerr black hole ($y=0,\ a^2=0.99;\ \ell\approx\ell_{\rm mb}$) and the Schwarzschild black hole ($y=0,\ a=0;\ \ell\approx\ell_{\rm mb}$), right picture depicts thick marginally bound accretion discs orbiting the KdS black hole ($y=10^{-6},\ a^2=0.99;\ \ell=\ell_{\rm 