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Microsecond wavelength secret of antisymmetric 5D black hole of infinity: Gerard 't Hooft Netflix
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Netflix infinity documentary
Quantum clones inside black holes
Nobel Physicist Gerard t Hooft
A systematic procedure is proposed for better understanding the evolution laws of black holes in terms of pure quantum states. We start with the two opposed regions I and II in the Penrose diagram, and study the evolution of matter in these regions, using the algebra derived earlier from the Shapiro effect in quantum particles. Since this spacetime has two distinct asymptotic regions, one must assume that there is a mechanism that reduces the number of states. In earlier work we proposed that region II describes the angular antipodes of region I, the `antipodal identification', but this eventually leads to contradictions. Our much simpler proposal is now that all states defined in region II are exact quantum clones of those in region I. This indicates more precisely how to restore unitarity by making all quantum states observable, and in addition suggests that generalisations towards other black hole structures will be possible. An apparent complication is that the wave function must evolve with a purely antisymmetric, imaginary-valued Hamiltonian, but this complication can be well-understood in a realistic interpretation of quantum mechanics.
"The Hawking particles are dominated by a tenuous cloud of particles with masses and energies far below the Planck value, so that, for the outside world, their direct effects on the total metric are negligible, though they will be important when considered over long stretches of time."
"Figure 1 shows that the regions III and IV play no role in the evolution at all.
The Cauchy surface is indicated there with a grey line. The clones move along with the dashed grey line. This line always pivots around the origin, so that III and IV are avoided. This is why we say that the black hole has no interior; regions III and IV are to be regarded as analytic extensions such as the analytic continuation towards complex coordinates, which are very useful for solving mathematical equations, but do not have
any direct physical interpretation."
"If one wants to talk about the black hole interior, one may consider region II as the interior, but we add to this that the interior contains nothing but clones of the real physical variables."
"An apparent complication is that the wave function must evolve with a
purely antisymmetric, imaginary-valued Hamiltonian, but this complication
can be well-understood in a realistic interpretation of quantum mechanics."
"From a fundamental point of view, demanding a wave function to be real is easy: just ensure that the Hamiltonian is imaginary, and hence antisymmetric."
"As the Hamiltonian must be imaginary and antisymmetric, the wave function in the entire region II is a quantum clone of that in region I ."
"In- and out-particles can punch through a horizon at positive values of u± (region I ), or negative u± (region II )."
"We see that the in-particles punch through the future event horizon either at positive u+ (region I ) or at negative u+ (region II ), see Figure 1. This ?figure is a Penrose diagram, obtained by squeezing the coordinates u± to fit in finite segments, in order to render the entire surrounding universe. The coordinates u± both span the entire line [−∞, ∞]."
"An observer close to the intersection point of the future event horizon and the past event horizon, defines the local energy and momentum density in terms of locally flat coordinates. (S)he then experiences a local vacuum there, which is a unique vacuum state, so that, from her point of view, we are dealing with a single pure state. We now borrow this language to say that, also for the outside observers, this may be regarded as a single pure state. We claim that any observer will not be able to distinguish a thermal state from a pure state in thermal equilibrium (a micro-canonical ensemble), so here comes our first postulate: The state where the local observer sees a local minimum of the energy density, i.e. a local vacuum state, will here be referred to as the Unruh vacuum state [3]; it may be regarded as a pure state. The excited states that we shall use, will in general be time dependent, small deviations from the Unruh state"
"Since the local observer sees no particles at all, Einstein’s equations will require that continuation be carried out by assuming strict absence of matter near the black hole. In particular, local observers will see no matter crossing future and past horizons"
"Eq.(4.1) was first derived in flat space-time [6], but it is easy to generalise it to the space-time (3.4) very close to a black hole horizon [7]"
the in-particles are defined by their momenta as they cross the future event horizon. light cone)momentum p− increases proportionally to eτ , where τ if the time coordinate for the outside observer, normalised as ...Similarly, out-particles have momenta p+ decreasing as e−τ ."
Quantum clones inside black holes
Nobel Physicist Gerard t Hooft
A systematic procedure is proposed for better understanding the evolution laws of black holes in terms of pure quantum states. We start with the two opposed regions I and II in the Penrose diagram, and study the evolution of matter in these regions, using the algebra derived earlier from the Shapiro effect in quantum particles. Since this spacetime has two distinct asymptotic regions, one must assume that there is a mechanism that reduces the number of states. In earlier work we proposed that region II describes the angular antipodes of region I, the `antipodal identification', but this eventually leads to contradictions. Our much simpler proposal is now that all states defined in region II are exact quantum clones of those in region I. This indicates more precisely how to restore unitarity by making all quantum states observable, and in addition suggests that generalisations towards other black hole structures will be possible. An apparent complication is that the wave function must evolve with a purely antisymmetric, imaginary-valued Hamiltonian, but this complication can be well-understood in a realistic interpretation of quantum mechanics.
"The Hawking particles are dominated by a tenuous cloud of particles with masses and energies far below the Planck value, so that, for the outside world, their direct effects on the total metric are negligible, though they will be important when considered over long stretches of time."
"Figure 1 shows that the regions III and IV play no role in the evolution at all.
The Cauchy surface is indicated there with a grey line. The clones move along with the dashed grey line. This line always pivots around the origin, so that III and IV are avoided. This is why we say that the black hole has no interior; regions III and IV are to be regarded as analytic extensions such as the analytic continuation towards complex coordinates, which are very useful for solving mathematical equations, but do not have
any direct physical interpretation."
"If one wants to talk about the black hole interior, one may consider region II as the interior, but we add to this that the interior contains nothing but clones of the real physical variables."
"An apparent complication is that the wave function must evolve with a
purely antisymmetric, imaginary-valued Hamiltonian, but this complication
can be well-understood in a realistic interpretation of quantum mechanics."
"From a fundamental point of view, demanding a wave function to be real is easy: just ensure that the Hamiltonian is imaginary, and hence antisymmetric."
"As the Hamiltonian must be imaginary and antisymmetric, the wave function in the entire region II is a quantum clone of that in region I ."
"In- and out-particles can punch through a horizon at positive values of u± (region I ), or negative u± (region II )."
"We see that the in-particles punch through the future event horizon either at positive u+ (region I ) or at negative u+ (region II ), see Figure 1. This ?figure is a Penrose diagram, obtained by squeezing the coordinates u± to fit in finite segments, in order to render the entire surrounding universe. The coordinates u± both span the entire line [−∞, ∞]."
"An observer close to the intersection point of the future event horizon and the past event horizon, defines the local energy and momentum density in terms of locally flat coordinates. (S)he then experiences a local vacuum there, which is a unique vacuum state, so that, from her point of view, we are dealing with a single pure state. We now borrow this language to say that, also for the outside observers, this may be regarded as a single pure state. We claim that any observer will not be able to distinguish a thermal state from a pure state in thermal equilibrium (a micro-canonical ensemble), so here comes our first postulate: The state where the local observer sees a local minimum of the energy density, i.e. a local vacuum state, will here be referred to as the Unruh vacuum state [3]; it may be regarded as a pure state. The excited states that we shall use, will in general be time dependent, small deviations from the Unruh state"
"Since the local observer sees no particles at all, Einstein’s equations will require that continuation be carried out by assuming strict absence of matter near the black hole. In particular, local observers will see no matter crossing future and past horizons"
"Eq.(4.1) was first derived in flat space-time [6], but it is easy to generalise it to the space-time (3.4) very close to a black hole horizon [7]"
the in-particles are defined by their momenta as they cross the future event horizon. light cone)momentum p− increases proportionally to eτ , where τ if the time coordinate for the outside observer, normalised as ...Similarly, out-particles have momenta p+ decreasing as e−τ ."
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