these spacetimes. In a SFBH spacetime as well as in a Schwarzschild spacetime, the effective potential of a test particle vanishes at the horizon and has, for sufficiently large $J$, at least one minimum and one maximum outside the horizon. The radius $r_{\!\scriptscriptstyle h}$ of the event horizon of a SFBH is always less than that of the vacuum black hole with the same mass (see Fig \[fig1\]). It follows directly from (\[asymp2\]) that $r_{\!\scriptscriptstyle h}\rightarrow0$ as $m\rightarrow\xi(0)/3+0$ and can be arbitrary close to zero. Moreover, the various numerical simulations with SFBH solutions allow us to conclude that the radius of the corresponding innermost stable circular orbit, which is an important observational characteristic for black holes, is of order $3r_{\!\scriptscriptstyle h}$ (analogously to the vacuum case). On the contrary, a SFNS has no innermost stable circular orbit but has a unique degenerated *static orbit*, which has $J=0$ and is located at $r=r_0$, where $r_0$ is the unique solution of the equation $A'(r)=0$. From the point of view of a distant observer resting relative to the centre, a test particle remains at rest in the static orbit all time. Particles in such a static orbit, together with particles having zero or 