How to calculate the gravitational force of a black hole outside event horizon at a given distance $r$? Let $g_{bh}$ $[kg·\frac{m}{s^2}]$ be the force caused by the gravity of a black hole.
How do we calculate the force $g_{bh}(r)$ outside event horizon $R_{Sch} = \frac{2GM}{c^2}$  onto a satellite with mass $m$ at a given distance $r$ from that black hole?
And with that formula, is it possible to also derive the speed $v_s$ of this satellite around that black hole (also outside event horizon $R_{Sch}$)? If yes, how?
 A: I will answer the second question first as I find it easier one on the computations and since the calculation for the first question is similar, I will only comment on it and leave the details for you.
First of all, there are no stable circular orbits under $r=3r_s$ and no circular orbits under $r=3r_s/2$ for Schwarzschild black hole.
Now, the worldline of satellite on circular orbit is $x^\mu(t)=(t,r,\pi/2,\omega t)$, where $\omega$ is angular velocity in Schwarschild coordinates. We can thus compute 4-velocity:
$$v^\mu=\frac{dx^\mu}{d\tau}=(1,0,0,\omega)\frac{dt}{d\tau},$$
where $\tau$ is proper time along the curve, i.e.:
$$d\tau^2=g_{tt}dt^2+g_{\phi\phi}\omega^2dt^2=dt^2\left(g_{tt}+g_{\phi\phi}\omega^2\right).$$
Thus the 4-velocity is:
$$v^\mu=\frac{dx^\mu}{d\tau}=(1,0,0,\omega)\frac{1}{\sqrt{g_{tt}+g_{\phi\phi}\omega^2}}.$$
Note the 4-velocity in these coordinates is constant. Therefore the 4-acceleration is simply given by Christoffel symbols:
$$a^\lambda=\Gamma^\lambda_{\nu\mu}v^\mu v^\nu.$$
We are interested in nonzero components, so only in $\Gamma^\lambda_{tt}$, $\Gamma^\lambda_{t\phi}$, $\Gamma^\lambda_{\phi t}$, $\Gamma^\lambda_{\phi\phi}.$You can google or compute that out of these the only nonzero are
$$\Gamma^r_{tt}=-\frac{r_s}{2r^2}g_{tt}$$
$$\Gamma^r_{\phi\phi}=r g_{tt}$$
Of course circular orbit is geodesic, so there is no acceleration. Therefore we demand:
$$0=\Gamma^r_{tt}v^t v^t+\Gamma^r_{\phi\phi}v^\phi v^\phi$$
and use this to compute $\omega:$
$$0=-\frac{r_s}{2r^2}+\omega^2r \Rightarrow \omega=\sqrt{\frac{r_s}{2r^3}}.$$
Now the velocity of orbiting depends on the observer. If we take observer at rest in schwarzshild coordinates, this one will measure velocity to be:
$$v=\frac{\sqrt{g_{\phi\phi}}d\phi}{\sqrt{-g_{tt}}dt}=\omega\sqrt{\frac{g_{\phi\phi}}{-g_{tt}}}=\sqrt{\frac{r_s}{2r^3}\frac{r^2}{1-\frac{r_s}{r}}}=\sqrt{\frac{r_s}{2(r-r_s)}}.$$
As you can see, this will give you speed of light $v=1$ for $r=3r_s/2$. So this is the closest circular orbit that can exist.
Now you can do the same computation to get gravitational "force" at some distance $r$. But first realize, there is no gravitational force in GR. But there is an acceleration. So you can compute 4-acceleration of some object the same way I just did and than look what kind of force is producing this acceleration. If this object is at rest w.r.t. black hole (i.e. follows the worldline $x^\mu(t)=(t,0,0,0)$ in Schwarzschild coordinates) this force needed to keep the object at place will represent how strong of a pull the gravitation exerts on the object, even though conceptually this is not what is really happening. I leave the computation to you.
