Origin of BH Entropy & Info Missing Puzzle Resolution

In summary, my interpretation of the origin of BH entropy is based on an exact solutions family to the Einstein equation sourced by a representing dust gas. The outside part of the solution is exactly Schwarzschild type. But its inside part is characterised by an initial radial mass profile M(rho) and a following ``collapsing’’ function a(tau,rho) which I called Over Cross Oscillation. Schematically, the solutions family can be written as,ds^2=-dtau^2+F(tau,M[rho])drho^2+a[…]^2rho^2dOmega^2 ……(1)OCO
  • #1
sufive
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TL;DR Summary
A unifying resolution to the problem of black hole entropy's origin and information missing puzzle
Dear everyone, I wish to discuss in this thread a classic/semi-classic interpretation on the origin of Bekenstein-Hawking entropy and the related resolution to Hawking's information missing puzzle, which were published in Nucl.Phys.B977 (2022) 115722 and Nucl.Phys.B990 (2023) 116171 after strictly executed peer review. I myself believe it's the most possible final resolution to these two key questions in theoretical black hole physics. But of course I would like to accept your critics if your critics hit the point indeed.

My interpretation for the origin of BH entropy is based on an exact solutions family to the Einstein equation sourced by a representing dust gas. The outside part of the solution is exactly Schwarzschild type. But its inside part is characterised by an initial radial mass profile M(rho) and a following ``collapsing’’ function a(tau,rho) which I called Over Cross Oscillation. Schematically, the solutions family can be written as,

ds^2=-dtau^2+F(tau,M[rho])drho^2+a[…]^2rho^2dOmega^2 ……(1)

OCO means that, when two dust particles hit on the central point, the east semi-sphere incomer over crosses to the west semi-sphere and vice versa. Both of them do not stay there or become a part of the previously formed singularity. This solution does not break the singularity theorem but resolves the conventionally understood singularity from a once and for all (eternal) one into a periodically forming and resolving one.

Through a canonic quantisation of the Einstein equation under the metric ansatz (1), I got a wave functional description of the dust ball, which I called as OCO fuzzball due to its horizon’s being blurred by the quantum fluctuation. At the same time, I found that after the quantisation, both the classically arbitrary initial mass profile M[rho] and the oscillation modes a[tau] becomes discrete and countable, with the degeneracy exactly consistent with the area law formula of BH entropy. This way, I claim that I got a classic or semi-classic interpretation for the origin of BH entropy.

With my interpretation for the BH entropy, the black hole becomes a completely normal object, just like the usual atom with inner structures. This allows me to study its gravity induced spontaneous radiation (which I shortened as GISR) through an explicitly hermitian hamiltonian,

H=H_bh+H_vac+H_int ……(2)

the first part is chosen as a diagonal matrix which represents all microscopic states of the black hole with various masses. The second part describes the vacuum fluctuation around the black hole which is represented by many harmonic oscillators. The third part couples the vacuum fluctuation modes and microscopic states of the black hole so that, every time a vacuum mode gets on shell, the black hole transitions between two special modes at a corresponding probability amplitude.

I proved that due to the exponential degeneracy of the black hole's microscopic state, the spectrum of GISR(2) is exactly of the thermal type and has exactly the same temperature as hawking radiation. For this reason, I argue that GISR is the underlying mechanism of hawking radiation. But because it is described by an explicitly hermitian hamiltonian, it involves no information missing and has the desired feature of Page curve when I compute the entropy of the black hole or the radiation particles.

Although GISR involves information missing, it makes the cause of information missing in Hawking’s argument transparent. The cause has two aspects: (i) exact thermal spectrum is only an instantaneous feature of GISR. A full evaporation evolution of a black hole is a non-equilibrium process and is characterised by a time dependent temperature curve. For different microscopic initial black hole, this curve is different. Hawking’s calculation gives up this feature completely. (ii) Hawking’s argument takes the evaporating black hole as a classic object with time dependent mass and neglects the entanglement superposition of different mass black holes and the corresponding radiation particles. That is, the proper middle state of the system should be written as

Psi[BH(t)]= BH_0*HwkPtcl_none+BH_big*HwkPtcl_little+BH_mid*HwkPtcl_some+... (3)

The superposition (3) looks very much like the state of dead+living cat in Schrodinger’s gedanken experiment. It is a must be in a full quantum treatment of a black hole’s radiation evolution. But in Hawking’s argument for information missing puzzle, it is neglected and the middle state of the black hole is written as
Psi[BH(t)]=BH_mass(t) (4)
 

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  • #2
sufive said:
which were published in Nucl.Phys.B977 (2022) 115722 and Nucl.Phys.B990 (2023) 116171
Please give links to the actual publication pages.
 
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  • #4
I have looked at the paper you attached and it looks nonsensical to me at several levels. Let me just focus on one thing. In Eq. (16) you describe evolution as a series of Penrose diagrams. But each Penrose diagram is a spacetime diagram, meaning that each Penrose diagram describes an evolution by itself. So how can evolution be described by a series of Penrose diagrams?
 
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  • #5
I notified in the paper after eq(17) that `` where PC-diagram with different length of zigzag part denotes different size black holes and their corresponding radiation products''. So the Penrose diagram in eq(16) is not the usual diagram you understood denoting an evolving space-time.
 
  • #6
In the Appendix you seem to say that horizon is not needed for Hawking radiation. I would recommend you to read https://arxiv.org/abs/hep-th/0106111 which points out that event horizon is not needed, but apparent horizon is needed. Neutron star, in particular, does not have an apparent horizon and hence cannot produce Hawking radiation.
 
  • #7
Thank you very much for the recommendation of papers, I will read it. On the question of hawking radiation needs/not horizon, my viewpoint is that: hawking radiation is a result but not a mechanism. This result says that the fixed position observers can measure particles from the vacuum defined by the freely falling observers. But its underlying mechanism is unknown. If the gravity induced spontaneous radiation is the underlying mechanism as I argue, then the horizon is not need for it.
 

FAQ: Origin of BH Entropy & Info Missing Puzzle Resolution

What is black hole entropy?

Black hole entropy is a measure of the amount of information or disorder associated with a black hole. It is typically expressed in terms of the area of the event horizon of the black hole, according to the Bekenstein-Hawking formula, which states that the entropy (S) is proportional to the area (A) of the event horizon divided by the Planck length squared: S = kA/4l_p², where k is the Boltzmann constant and l_p is the Planck length.

How does black hole entropy relate to thermodynamics?

Black hole entropy is analogous to the entropy in thermodynamics, where it quantifies the number of microstates corresponding to a macrostate. Just as thermodynamic systems have temperature, pressure, and volume, black holes have temperature (related to their surface gravity) and entropy, leading to the interpretation of black holes as thermodynamic systems. This relationship has profound implications for the nature of gravity and quantum mechanics.

What is the information paradox associated with black holes?

The information paradox arises from the conflict between quantum mechanics and general relativity. According to quantum mechanics, information must be preserved, but when matter falls into a black hole, it seems to be lost forever when the black hole evaporates via Hawking radiation. This leads to the question of whether the information about the initial state of matter is irretrievably lost, which challenges our understanding of fundamental physics.

What are some proposed resolutions to the black hole information paradox?

Several resolutions have been proposed, including the idea that information is somehow encoded in the Hawking radiation emitted by black holes, allowing it to be recovered. Other theories suggest that information may be stored on the event horizon (the holographic principle) or that black holes could lead to alternate universes. Some physicists also propose that the laws of quantum mechanics may need to be modified to accommodate the peculiar nature of black holes.

Why is the origin of black hole entropy significant for physics?

The origin of black hole entropy is significant because it connects quantum mechanics, thermodynamics, and gravity, leading to a deeper understanding of fundamental physical laws. It challenges existing theories and encourages the development of a unified framework that reconciles general relativity and quantum mechanics, which is essential for advancing our understanding of the universe and the nature of reality.

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