On 1/14/2018 5:30 AM, Lawrence Crowell wrote:
On Saturday, January 13, 2018 at 6:30:33 PM UTC-6, Brent wrote:
On 1/13/2018 2:44 PM, agrays...@gmail.com <javascript:> wrote:
On Saturday, January 13, 2018 at 2:59:00 PM UTC-7, Brent wrote:
Classically, the radiation isn't "trapped"; it goes to the
singularity (what the QM does? dunno). The inflowing
radiation is just that starlight that falls on the event
horizon...which is not particularly bright.
Brent
I'm referring to the INTERIOR of the BH.
So am I.
If the radiation is trapped inside, the environment is likely hot
and bright.
Or it's absorbed by the singularity...or whatever is really
there. There's not reasonable picture in which it is "trapped
inside" and is flying around inside the black hole. Inside a
Schawarzschild black hole "the singularity" is on the future of
every world line, including null ones. Inside a Kerr-Newman black
hole it may be possible to miss "the singularity" but then it
appears to connect to a another spacetime. Both of these are
solutions for eternal black holes, so when it's a black hole that
forms and then evaporates the solutions may not hold. However,
except near "the singularity" the analyses would hold and so
except for within nanoseconds of "the singularity" all photons are
going to be traveling toward "the singularity" and not flying
around willy-nilly, "trapped" in the black hole. They can't turn
around because that direction is the past.
Brent
This of course gets a bit weird. I put in a short Penrose diagram of
the Kerr-Newman black hole. Matter on the right I region will cross
the r_+ horizon and fall into the III spacelike region. From there it
must cross the interior horizon at r_-. Now there are two funny points
here. The first is whether the r_- horizon is a mass inflation
singularity and prevents any information from crossing.
But have you seen this paper:
Mass inflation inside black holes revisited
Vyacheslav I. Dokuchaev
(Submitted on 1 Sep 2013 (v1), last revised 21 Feb 2014 (this version, v4))
The mass inflation phenomenon implies that black hole interiors are
unstable due to a back-reaction divergence of the perturbed black hole
mass function at the Cauchy horizon. Weak point in the standard mass
inflation calculations is in a fallacious using of the global Cauchy
horizon as a place for the maximal growth of the back-reaction
perturbations instead of the local inner apparent horizon. It is derived
the new spherically symmetric back-reaction solution for two
counter-streaming light-like fluxes near the inner apparent horizon of
the charged black hole by taking into account its separation from the
Cauchy horizon. In this solution the back-reaction perturbations of the
background metric are truly the largest at the inner apparent horizon,
but, nevertheless, remain small. The back reaction, additionally,
removes the infinite blue-shift singularity at the inner apparent
horizon and at the Cauchy horizon.
(or arXiv:1309.0224v4 [gr-qc] for this version)
Brent
The other is a spatial surface in the cosmology region I has two
alternatives that connect to two inner timelike regions IV and V. This
illustrates some possible monodromy associated with the interior of a
black hole.
The prospect of this monodromy raises the question of whether these
inner regions IV and V are in some ways entangled with quantum states
in the exterior region. There then might be some physical region there
instead of just this being a mathematical idealization. If so this
interior region is filled with radiation and particles on closed
timelike curves cycling around the singularity. The real question of
course is whether there is some entanglement of states between the
regions I and II, two timelike regions that may have multiverse
considerations, and whether the ambiguity of how one pushes a
spacelike surface forwards means there are also entanglements in the
two interior regions.
LC
<https://lh3.googleusercontent.com/-LFRNH9NhvUg/WltY3b6FPtI/AAAAAAAADNI/nXma0OO04KQPjLnzq9W3_Jv45DnffpcfgCLcBGAs/s1600/Penrose%2Bdiagram%2Bfor%2BRN%2Bwith%2B2%2Bspatial%2Bsurfaces.png>
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