awking evaporation and the fate of black holes in loop quantum gravity Idrus Husin Belfaqih,1, ∗ Martin Bojowald,2, † Suddhasattwa Brahma,1, ‡ and Erick I. Duque2, § 1Higgs Centre for Theoretical Physics, School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3FD, UK 2Institute for Gravitation and the Cosmos, The Pennsylvania State University The evaporation process: The emission rate slows down at a sub-Planckian mass Mr , suggesting a sta- ble remnant.
Conclusions: As the mass of an evaporating LQG black hole shrinks toward Mr , holonomy corrections dramati- cally slow down Hawking radiation. When the horizon area reaches a Planckian size, quantum fluctuations can no longer be ignored. Within fluctuations, the horizon reaches the minimum-area reflection-symmetry surface at Mf > Mr . In the underlying quantum state, there is a finite probability for a sub-Planckian black hole to tunnel into a white hole [33], an outcome that would al- ways be preferred given that it takes a long time to form the remnant at mass Mr . Going beyond heuristic claims, we provide a physical mechanism, based on a holonomy- induced instability in a quasi-normal mode which consti- tutes an explicit candidate for an initial white-hole emis- sion at a mass scale Mc > Mr . Crucially, the mass hier- archy Mr < Mc < Mf derived here reveals that the black hole first turns quantum, as shown by significant quan- tum fluctuations at Mf , and forms a superposition of a horizon-covered black hole with an exposed white hole. This stage is followed by the quantum-gravitational in- stability triggering an explosion at Mc, well before Hawk- ing radiation starts weakening at Mr . Our results provide the first covariant, self-consistent
White holes are a wildly speculative concept. There is no evidence that they exist and there should be evidence that they exist if they do given the extent of of astronomy observations. Like traversable black holes, it is a litmus test of papers that shouldn't be taken seriously as descriptions of reality.
but there is "As the mass of an evaporating LQG black hole shrinks toward Mr , holonomy corrections dramati- cally slow down Hawking radiation. When the horizon area reaches a Planckian size, quantum fluctuations can no longer be ignored.The evaporation process: The emission rate slows down at a sub-Planckian mass Mr , suggesting a sta- ble remnant."
opinions of [Submitted on 23 Apr 2025] Hamiltonian quantization of complex Chern-Simons theory at level-k Muxin Han
This paper develops a framework for the Hamiltonian quantization of complex Chern-Simons theory with gauge group SL(2,C) at an even level k∈Z+. Our approach follows the procedure of combinatorial quantization to construct the operator algebras of quantum holonomies on 2-surfaces and develop the representation theory. The ∗-representation of the operator algebra is carried by the infinite dimensional Hilbert space Hλ⃗ and closely connects to the infinite-dimensional ∗-representation of the quantum deformed Lorentz group Uq(sl2)⊗Uq˜(sl2), where q=exp[2πik(1+b2)] and q˜=exp[2πik(1+b−2)] with |b|=1. The quantum group Uq(sl2)⊗Uq˜(sl2) also emerges from the quantum gauge transformations of the complex Chern-Simons theory. Focusing on a m-holed sphere Σ0,m, the physical Hilbert space Hphys is identified by imposing the gauge invariance and the flatness constraint. The states in Hphys are the Uq(sl2)⊗Uq˜(sl2)-invariant linear functionals on a dense domain in Hλ⃗ . Finally, we demonstrate that the physical Hilbert space carries a Fenchel-Nielsen representation, where a set of Wilson loop operators associated with a pants decomposition of Σ0,m are diagonalized.
Comments: 52 pages, 10 pages appendix, 4 figures Subjects: High Energy Physics - Theory (hep-th); General Relativity and Quantum Cosmology (gr-qc); Quantum Algebra (math.QA) Cite as: arXiv:2504.16367 [hep-th]
6 comments:
I'm tempted to make up a poster with that and post it on my office door.
It's worthy.
awking evaporation and the fate of black holes in loop quantum gravity
Idrus Husin Belfaqih,1, ∗ Martin Bojowald,2, † Suddhasattwa Brahma,1, ‡ and Erick I. Duque2, §
1Higgs Centre for Theoretical Physics, School of Physics and Astronomy,
University of Edinburgh, Edinburgh EH9 3FD, UK
2Institute for Gravitation and the Cosmos, The Pennsylvania State University
The evaporation process: The emission rate slows
down at a sub-Planckian mass Mr , suggesting a sta-
ble remnant.
Conclusions: As the mass of an evaporating LQG black
hole shrinks toward Mr , holonomy corrections dramati-
cally slow down Hawking radiation. When the horizon
area reaches a Planckian size, quantum fluctuations can
no longer be ignored. Within fluctuations, the horizon
reaches the minimum-area reflection-symmetry surface
at Mf > Mr . In the underlying quantum state, there
is a finite probability for a sub-Planckian black hole to
tunnel into a white hole [33], an outcome that would al-
ways be preferred given that it takes a long time to form
the remnant at mass Mr . Going beyond heuristic claims,
we provide a physical mechanism, based on a holonomy-
induced instability in a quasi-normal mode which consti-
tutes an explicit candidate for an initial white-hole emis-
sion at a mass scale Mc > Mr . Crucially, the mass hier-
archy Mr < Mc < Mf derived here reveals that the black
hole first turns quantum, as shown by significant quan-
tum fluctuations at Mf , and forms a superposition of a
horizon-covered black hole with an exposed white hole.
This stage is followed by the quantum-gravitational in-
stability triggering an explosion at Mc, well before Hawk-
ing radiation starts weakening at Mr .
Our results provide the first covariant, self-consistent
White holes are a wildly speculative concept. There is no evidence that they exist and there should be evidence that they exist if they do given the extent of of astronomy observations. Like traversable black holes, it is a litmus test of papers that shouldn't be taken seriously as descriptions of reality.
but there is "As the mass of an evaporating LQG black
hole shrinks toward Mr , holonomy corrections dramati-
cally slow down Hawking radiation. When the horizon
area reaches a Planckian size, quantum fluctuations can
no longer be ignored.The evaporation process: The emission rate slows
down at a sub-Planckian mass Mr , suggesting a sta-
ble remnant."
Planckian mass stable remnant as dark matter
mitchell porter
opinions of [Submitted on 23 Apr 2025]
Hamiltonian quantization of complex Chern-Simons theory at level-k
Muxin Han
This paper develops a framework for the Hamiltonian quantization of complex Chern-Simons theory with gauge group SL(2,C) at an even level k∈Z+. Our approach follows the procedure of combinatorial quantization to construct the operator algebras of quantum holonomies on 2-surfaces and develop the representation theory. The ∗-representation of the operator algebra is carried by the infinite dimensional Hilbert space Hλ⃗ and closely connects to the infinite-dimensional ∗-representation of the quantum deformed Lorentz group Uq(sl2)⊗Uq˜(sl2), where q=exp[2πik(1+b2)] and q˜=exp[2πik(1+b−2)] with |b|=1. The quantum group Uq(sl2)⊗Uq˜(sl2) also emerges from the quantum gauge transformations of the complex Chern-Simons theory. Focusing on a m-holed sphere Σ0,m, the physical Hilbert space Hphys is identified by imposing the gauge invariance and the flatness constraint. The states in Hphys are the Uq(sl2)⊗Uq˜(sl2)-invariant linear functionals on a dense domain in Hλ⃗ . Finally, we demonstrate that the physical Hilbert space carries a Fenchel-Nielsen representation, where a set of Wilson loop operators associated with a pants decomposition of Σ0,m are diagonalized.
Comments: 52 pages, 10 pages appendix, 4 figures
Subjects: High Energy Physics - Theory (hep-th); General Relativity and Quantum Cosmology (gr-qc); Quantum Algebra (math.QA)
Cite as: arXiv:2504.16367 [hep-th]
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