## ? on entrop of black holes

My physics professor told us that string theory correctly predicts the entropy ofa black hoole. that leaves me wondering...how do u even measure what it's entropy is to even confirm a theoreticla calculation?

is S= k ln W even used at all?
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 Quote by RasslinGod My physics professor told us that string theory correctly predicts the entropy ofa black hoole. that leaves me wondering...how do u even measure what it's entropy is to even confirm a theoreticla calculation? is S= k ln W even used at all?
As far I know, this relation has been used only for "exotic" black holes, i.e., black holes that have one or more of supersymmetry, Yang-Mills charge, and extra macroscopic spatial dimensions.

Also as far as I know, astrophysical black holes have none of these properties.

## ? on entrop of black holes

Recently people in strings have been doing non-supersymmetric as well.. of course these are not even close to astorphysical black holes...
 There is the Hawking-Unruh effect, which tend to merge in a way for an accelerated frame near a black hole. To examine this it is best to transform to another set of coordinates to look at this. The Kruskal-Szekeres coordinates are better. These are given by $$u~=~\sqrt(r/2M - 1)e^{r/4M}cosh(t/2M),$$ $$v~=~\sqrt(r/2M - 1)e^{r/4M}sinh(t/2M).$$ It is clear that $$(r/2M~-~1)e^{r/2M}~=~u^2~-~v^2$$ and $$tanh(t/4M)~=~v/u.$$ This has the advantage that there is no funny business at $r~=~2M$. These coordinates provide a chart which covers the whole space. The $u^2~-~v^2$ equation shows that the inner and outer regions of the black hole are given by a branch cut connecting two sheets. Consider $(r/2M~-~1)e^{r/2M}~=~x^2$, and so $x^2~=~u^2~-~v^2$. The u and v satisfy hyperbolic equations for a constant r and so $$u~=~sinh(gs),~ v~=~cosh(gs).$$ It is clear that for $udu~-~vdv~=~e^{r/2M}/4M dr$ that $g~=~1/(r/2M~-~1)e^{t/2M}/4M$ , and so the accleration diverges as $r~\itex~2m$ in order to hold a particle fixed near the event horizon. The hyperbolic equations above are then identical in form to the ones which obtain for the Unruh effect. The spacetime trajectory in the u and v coordinates is then hyperbolic. Thus for an observer sitting on a frame fixed next to the event horizon of the black hole there would be a huge thermal bath of particles which would become very hot $T~\rightarrow~\infty$ as $r~\rightarrow~2M$. The four velocities $U_u$ and $U_v$ will then satisfy $$U_u = 1/(4M(r/2M - 1))e^{t/2M}cosh(gs), U_v = 1/4M((r/2M - 1))e^{t/2M}sinh(gs),$$ with $$(U^u)^2~-~(U_v)^2~=~16M^2(1~-~r/2M)e^{-t/2M},$$ and so the temperature of the black hole is $T~\sim~1/2\pi g$ and $$T~=~\frac {e^{t/M}}{8\pi M}\sqrt{1~-~r/2M}).$$ Now for $r~\rightarrow~\infty$ and $t~\rightarrow~\infty$ this recovers the standard black hole temperature result of $$T~=~\frac{1}{8\pi M}.$$ Thus for an observer held close to the event horizon of a black the additional acceleration effectively heats up the black hole on that frame. I think this might also indicate that for a distant observer there is a question as to what she would see of her compatriot held fixed near the black hole. This might be an interesting problem to examine.
 I made a couple of Tex errors on the above discussion which I corrected L. C.

 Quote by George Jones As far I know, this relation has been used only for "exotic" black holes, i.e., black holes that have one or more of supersymmetry, Yang-Mills charge, and extra macroscopic spatial dimensions. Also as far as I know, astrophysical black holes have none of these properties.
These exotic black holes are BPS black holes, and pertain to issues of quantum gravity or dualities between D-branes and gauge charges. The astrophysical black hole is massive and these putative physics are in some infinitesimal region (or a small number of Planck lengths) from the event horizon. Hence for a stellar black hole these BPS things don't contribute much of anything.

Lawrence B. Crowell