Maximal kinetic energy due to gravitational attraction Two related questions:


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*Small object of mass $m$ is falling into the supermassive black hole of mass $M$. What is the maximal kinetic energy can be acquired by the small object, from the point of view of an observer  whose frame of reference is at rest   near event horizon?
Can it exceed $(M+m)c^2$?

*Two small black holes of equal mass $M$ are attracted each other. 
What is the maximal kinetic energy can be acquired by each black hole due to gravitational attraction, from the point of view of an observer between them?
 A: For case 1) The energy is well-defined, and it can be shown that (for the case of a Schwarzschild hole, but this can be generalized to a spinning charged hole if you wish):
$$-1 = \frac{-E^{2} + {\dot r}^{2}}{1-\frac{2M}{r}} + \frac{L^{2}}{r^{2}}$$ holds for the entire motion of a test particle, where, for a test particle with mass $m$, $Em$ is the total energy of the orbit, and $Lm$ is the angular momentum of the orbit.  Answering your question is just a matter of applying it to this equation, but note that, as $L,r,{\dot r}\rightarrow 0$, you have $Em\rightarrow m$, which implies that the total energy of a stationary object far from the black hole is approximately its rest mass.
For 2), the case is very considerably more complicated.  You can get a first order guess by considering the Area increase theorem, which tells you that the two black holes will coalesce to a black hole whose area is no less than the sum of the previous two black holes' area, which gives you the inequality $M_{1}^{2} + M_{2}^{2} \leq M^{2}$, up to some factors involving the spin (if you want to factor spin), this then gives you a cap on how much net energy you can transfer into gravitational radiation and the final translational kinetic energy of the final black hole (which is possible, because the gravitational radiation can be asymmetric, and typically, uneven mass black holes will end up with a translational velocity that is something like $10^{-3}c$, which can be above escape velocity from the enclosing galaxy. 
Note that there are still bounds on this, because, since the spacetime will be asymptotically flat, the ADM Mass of the spacetime will be conserved. 
A: technically, it would be infinite, as the energy of an object is determined by -GMm/(2r)
A: The two objects have very low chance of moving directly onto each other.
The nearest orbit would be the sum of the two Schwartzschildradei of the objects.
1 r=2G(M+m)/c^2 if you put this in E=GMm/r you get Mmc^2/2(M+m)<=mc^2/2 
  For (m<

2 r=2G(M+M)/c^2 and you get E=Mc^2/4
From these distances they will become accretion objects. 
