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  • 2 weeks later...

I am not sure if this can be pulled off with our current equipment... but I need spectral analysis of star light passing through the radio source in SN1006 at RA 15 02 36 DEC -41 53 01, the Zeeman Effect is what I am after...

 

Also, a uniform weak Zeeman effect should be present in all star light emanating from elliptical galaxies, globular clusters, and the recently discovered globular galaxies.

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  • 2 weeks later...

I wrote my original paper last May and this was released to the public in late July:

http://news.sciencemag.org/space/2013/07/swirls-afterglow-big-bang-could-set-stage-major-discovery

That finding was later attacked.  http://www.nature.com/news/big-bang-blunder-bursts-the-multiverse-bubble-1.15346

 

This Paul Steinhardt guy, who is able to get articles published in Nature, does not like the Big Bang theory at all.

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  • 1 month later...

By merging two seemingly conflicting theories, Laura Mersini-Houghton has mathematically proven black holes can never come into being in the first place. Black holes are thought to be the densist matter in the universe.
 
Mersini-Houghton's theory combine Hawking's radiation theory with a fundamental law of quantum theory that states no information from the universe can ever disappear.
 
Mersini-Houghton agrees with Hawking in that a star's collapse gives off radiation; but by giving off radiation, she said the star also sheds mass to the point that it no longer has the density to become a black hole.

 

direct link to source paper: 

 

Arxiv - Back-reaction of the Hawking radiation flux on a gravitationally collapsing star II: Fireworks instead of firewalls

 

first 2 paragraphs of the papers introduction:

 

The backreaction of Hawking radiation on the evolu-
tion of the collapsing star is the most important problem
in the quantum physics of black holes. This problem
provides an arena for the interplay of quantum and grav-
itational eects on black holes and their respective im-
plications for the singularity theorem. A key feature of
Hawking radiation, which was well established in seminal
works by [3, 4, 9, 11, 17{20], is that the radiation is pro-
duced during the collapse stage of the star prior to black
hole formation. The very last photon making it to future
innity and thus contributing to Hawking radiation, is
produced just before an horizon forms. However its eect
on the collapse evolution of the star was considered for
the rst time only recently [1]. As was shown in [1] once
the backreaction of Hawking radiation is included in the
interior dynamics of the star, then the collapse stops and
the star bounces. Solving analytically for the combined
system of a collapsing star with the Hawking radiation
included, is quite a challenge. The system studied in [1]
was idealized in order to obtain an approximate analyti-
cal solution: there the star was taken to be homogeneous;
the star's fluid considered was dust; the star was placed
in a thermal bath of Hawking radiation which arises from
the time-symmetric Hartle-Hawking initial conditions on
the quantum eld in the far past. Within these approx-
imations, the main finding of [1] was that a singularity
and an horizon do not form after the star's collapse be-
cause the star reverses its collapse and bounces at a nite
radius due to the balancing pressure of the negative en-
ergy Hawking radiation in its interior. Yet, the evolution
of the star could not be followed beyond the bounce with
the approximate analytic methods of [1].
 
Given the fundamental importance of this problem and
the intriguing results of [1], we here aim to study the
backreaction of Hawking radiation on the collapsing star
by considering a more realistic setting, namely: we allow
the star to be inhomogeneous and consider an Hawking
radiation flux of negative energy which propagates in the
interior of the star, with its counterpart of positive energy 
flux travelling outwards to innity. Hawking radiation 
flux arises when the initial conditions imposed on the
quantum field on the background of the star, are chosen
to be in the Unruh vacuum state in the far past [9, 18]. In
contrast to the Hartle-Hawking initial state which leads
to an idealized time symmetric thermal bath of radia-
tion present before and after the collapse, the choice of
the Unruh vacuum describes a flux of thermal radiation
which is zero before the collapse and switches on after
the collapse. We solve numerically the full 4 dimensional
set of Einstein and of total energy conservation equations
leading to a complete set of hydrodynamic equations for
this model. Numerical solutions allows us to follow the
evolution of the collapsing star beyond its bounce.

 

 
Edited by Grames
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