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Jack Sarfatti proper acceleration in a static coordinate metric

ds^2 = gttdt^2 - grrdr^2 - r^2(spherical coordinate metric)


g(r) ~ gtt^-1/2d(g00/dr)

the two metrics of interest are

gtt = 1 - A^1/2/r black hole of area entropy A

we at r ---> infinity outside black hole

gtt = 1 - r'^2/A de Sitter horizon

we at r' = 0

inside cosmological horizon


1 + z = femit/fobserve f = frequency

1 + z = [gtt(observe)gtt(emit)]^1/2


Quantum gravity says horizons gtt = 0 are really Lp thick.

so for both metrics above using

r = A^1/2 + Lp for black hole


r' = A^1/2 - Lp

get same factors (Lp/A^1/2)^1/2 redshift of radiation emitted from A

(A^1/2/Lp)^1/2 blue shift of radiation falling into A.

Now the Hawking black hole radiation temperature at A is

T ~ h(A^1/2/Lp)c^2/cA^1/2kB ~ hc/kB(LpA^1/2)^1/2

and this redshifts down to hc/A^1/2kB ~ Newtonian horizon surface gravity just as Hawking says.

In contrast, for the new quantum gravity radial oscillations of the thickness of the horizon

T' ~ hc/LpkB

which redshifts down to us to T' ~ hc/kB(LpA^1/2)^1/2

by Stephan Boltzman T^4 law

this gives hc/Lp^2A

both for anomalous w = +1/3 radiation from black holes whose horizon is not observer dependent

& also dark energy density from future horizon which looks like w = -1 virtual photon vacuum energy peaked at c/(LpA^1/2)^1/2 frequency whose horizon is observer dependent.

We need to use John Cramer's TI here.

en.wikipedia.orgIn physics (especially astrophysics), redshift happens when light seen coming from an object that is moving away is proportionally increased in wavelength, or shifted to the red end of the spectrum. More generally, when an observer detects electromagnetic radiation outside the visible spectrum, "red...

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