HansH said:
if I understand that well you say that you cannot have influence on that because it always remains a moment in future.
No, that's not what I said. It's only a moment of time in your future if you are inside the hole. If you remain forever outside the hole, it's not. It's in a region of spacetime that becomes unreachable for you after a particular point on your worldline: the point at which your future light cone no longer includes any events inside the hole--or, in more ordinary language, the point after which you could no longer make yourself fall into the hole before it evaporated away even if you fell radially inward at the speed of light.
HansH said:
how does that relate to what is said in #10:
'The problem is that the math we use to calculate the rate of energy release makes some assumptions that probably do not hold as the mass of the hole goes all the way to zero.'
If we don't make those assumptions, we can't say anything about what happens because we don't have any other model of black hole evaporation to use. Everything I have said is using the model whose spacetime diagram I linked to, which is a model that is made using those assumptions.
Note, however, that there are other "black hole" models, such as the Bardeen "black hole" (a forum search on that term should turn up some previous threads on the topic), which aren't actually black holes at all (hence the scare quotes), because they don't have actual event horizons, only apparent horizons, and they don't have singularities. The objects in these models, however,
look like black holes from the outside, and also evaporate in a way similar to the way Hawking envisioned.
It is quite possible that, as our understanding of physics in this area improves, we will find that some model like that is actually the correct description for the objects that we now refer to as "black holes". That would be nice because it would remove all the issues associated with the presence of an event horizon and singularity in the model whose spacetime diagram I linked to above.