mb}$) and the SdS black hole ($y=10^{-6},\ a=0;\ \ell=\ell_{\rm mb}$).[]{data-label="f4"}](disks-jets.eps){width=".9\hsize"}

We can give to our results proper astrophysical relevance by presenting numerical estimates for observationally established current value of the RRCC[^2]. Having the value of $\Lambda_{0} \approx 1.3 \times 10^{-56}{\rm cm}^{-2}$, we can determine the mass parameter of the spacetime corresponding to any value of $y$, parameters of the equatorial circular geodesics and basic characteristics of both the thin and thick accretion discs (Table \[t1\]). Outer edge of the marginally bound thick accretion disc is determined by the outer marginally bound circular orbit which is located very close to, and for presented values of $y$ almost at the static radius of a given spacetime.

\[t1\]

It is well known[@Car-Ost:1996:ModAst:] that dimensions of accretion discs around stellar-mass black holes ($M
\sim 10 M_\odot$) in binary systems are typically $10^{-3}$pc, dimensions of large galaxies with central black-hole mass $M \sim 10^8 M_\odot$, of both spiral and elliptical type, are in the interval 50–100 kpc, and the extremely large elliptical galaxies of cD type with central black-hole mass $M \sim 3\times 10^9 M_\odot$ extend up to 1 Mpc. Therefore, we can conclude that the influence of the RRCC is quite negligible in the 