By Leonard Susskind
During the last decade the physics of black holes has been revolutionized through advancements that grew out of Jacob Bekenstein s attention that black holes have entropy. Stephen Hawking raised profound matters in regards to the lack of details in black gap evaporation and the consistency of quantum mechanics in a global with gravity. for 2 many years those questions wondered theoretical physicists and at last ended in a revolution within the approach we predict approximately area, time, subject and knowledge. This revolution has culminated in a impressive precept referred to as The Holographic precept , that's now a tremendous concentration of realization in gravitational study, quantum box conception and straightforward particle physics. Leonard Susskind, one of many co-inventors of the Holographic precept in addition to one of many founders of String concept, develops and explains those ideas.
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Additional info for An introduction to black holes, information and the string theory revolution : the holographic universe
As we have seen, the relativistic analogue of a uniformly accelerated frame is Rindler space. Because Rindler space covers only a portion of the space-time geometry (Region I) there are new and subtle features to the description of quantum ﬁelds. These features are closely associated with the existence of the horizon. The method we will use applies to any relativistic quantum ﬁeld theory including those with nontrivial interactions. For illustrative purposes we will consider a free scalar ﬁeld theory.
Quantum Fields in Rindler Space 41 8 ω= (a) (c) (b) 8 ω=− Fig. 4 Vacuum pair ﬂuctuations near the horizon A virtual ﬂuctuation is usually considered to be short lived because it “violates energy conservation”. If the virtual ﬂuctuation of energy needed to produce the pair is E, then the lifetime of the ﬂuctuation ∼ E −1 . Now consider the portion of the loop (b) which is found in Region I. From the viewpoint of the Fidos, a particle is injected into the system at ω = −∞ and ρ = 0. The particle travels to some distance and then falls back towards ρ = 0 and ω = +∞.
1) ρ=0 where T 00 is the usual Hamiltonian density used by the Minkowski observer. 2) where Π is the canonical momentum conjugate to χ. 3) The origin of the factor ρ in the Rindler Hamiltonian density is straightforward. 1 the relation between neighboring equal Rindler-time surfaces is shown. 4) Thus, to push the ω-surface ahead requires a ρ-dependent time translation. This is the reason that T 00 is weighted with the factor ρ. The Rindler Hamiltonian is similar to the generator of Lorentz boosts from the viewpoint of the Minkowski observer.
An introduction to black holes, information and the string theory revolution : the holographic universe by Leonard Susskind