Re: Black Hole Bouncing vs Evaporation vs Control

From: OsherD (mdoctorow_at_comcast.net)
Date: 03/01/05 

Date: 28 Feb 2005 23:05:37 -0800

>>From Osher Doctorow

Most of the energy of the star is concentrated in the core, while the
transition
region connects core and tail, and the tail has energy density
approaching 0.

The total energy of the system is conserved, and evaporation of the
collapsing
star occurs up to a rebound of the core in the high energy regime where
the
energy density is of order lambda, after which the system
anti-evaporates,
"possibly" back to its original state. The system is a collapsing dust
star or
rather collapsing-expanding dust star.

Let's back up into the Randall-Sundrum (RS) BraneWorld (BW) scenario,
from
which with some additions it was found by Bruni, Germani, and Maartens
in 2001
Phys. Rev. Lett. 87, 231-302, that unlike 4-dimensional GR the collapse
of
homogeneous stars leads to non-static exteriors. I should also mention
that the
Tolman geometry is used for the brane star because it has the only
spherically
symmetric metric preventing dissipation of energy across the shells of
the
collapsing star, so that Hawking radiation emits gravitons into the
bulk. The
Tolman geometry is also related to 5 dimensions, which dimensions are
the
usual ones plus the dimension of the "extra-dimensional" brane
coordinate y,
where the brane is located at y = 0. The Tolman geometry has to be
the
geometry of a spherically symmetric 4-dimensional slice (with dust) of
a 5-dimen-
sional diagonal metric.

I'll try to continue soon.

Osher Doctorow

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