In general for any null geodesic horizon observer-independent black hole, or observer-dependent cosmological dark energy (virtual bosons) de Sitter (dS, /\ > 0) or dark matter (virtual fermion-antifermion pairs) anti- de Sitter (AdS, /\ < 0) the Hawking temperature from the horizon is

THawking ~ hc|/\|^1/2/kBThe hologram entropy S of the horizon isS ~ kB/4|/\|Where, the hologram principle demands1/|/\| ~ NLp^2N = integer (Bekenstein BITS)Lp^2 ~ 10^-66 cmHeisenberg's uncertainty principle in 3D space changes to&x ~ h/&p + (&L)^2&p/hwhere&L ~ (Lp^2L)^1/3for measurement scale LNote for the max L of ~ 13.7 billion light years&L ~ 1 fermi 10^-13 cmand its minimum is LP ~ 10^-33 - only 20 powers of tenIn an S-Matrix scattering L ~ &p/h + ...infinite recursion, but approximately&x ~ h/&p + (Lp^2h/&p)^2/3&p/h~ h/&p + Lp^4/3(&p/h)^1/3&L is cube root of the quantum of volume in the 3D hologram image of the pattern of 2D Planck area BITs on our future dS horizon inAll of our Bohm explicate order 3D information is encoded nonlocally smeared as the 2D BIT pattern quantum Conway games at the intersection of our future light cone with our future dS horizon - we are at its perfect center. This is Bohm's implicate order! See Lenny Susskind's picture of the simpler black hole situation.This obey's t'Hooft's S-Matrix Unitarity.The tensor covariant non-geodesic acceleration magnitude is g, here we have an additional Unruh temperature since the quantum vacuum of an off-geodesic detector is not the same as a (timelike) geodesic detectorTUnruh ~ hg/ckBAdd the two temperatures.Outside a black hole the static LNIFs haveg = c^2(rs/2r^2)(1 - rs/r)^-1/2 ---> infinity at the horizoninside our future dS cosmic horizon hologram computer screen, we are at r = 0 and static LNIFs at distance r from us haveg = c^2/\^1/2(1 - /\r^2)^-1/2 ----> infinity at the horizonA = 1//\ ~ 10^123 Lp^2 ~ (14 billion light years)^2

Category: Physics

Published on Thursday, 11 March 2010 20:16

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