scholarly journals HAWKING RADIATION, GRAVITATIONAL ANOMALY, AND CONFORMAL SYMMETRY — THE ORIGIN OF UNIVERSALITY

2008 ◽  
Vol 23 (14n15) ◽  
pp. 2082-2090 ◽  
Author(s):  
SATOSHI ISO
Keyword(s):  
Black Hole ◽  
Hawking Radiation ◽  
Conformal Transformation ◽  
Conformal Symmetry ◽  
Black Hole Horizon ◽  
Gravitational Anomaly ◽  
Universal Behavior ◽  
Higher Spin ◽  
Matter Fields ◽  
Conformal Symmetries

The universal behavior of Hawking radiation is originated in the conformal symmetries of matter fields near the black hole horizon. We explain the origin of this universality based on (1) the gravitational anomaly and its higher-spin generalizations and (2) conformal transformation properties of fluxes.

From Schwarzschild to Kerr under de Sitter background due to blackhole tunnelling

2007 ◽  
Vol 85 (8) ◽  
pp. 863-868 ◽  
Author(s):  
K Xiao ◽  
W Liu
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Event Horizon ◽  
Hawking Radiation ◽  
Emission Rate ◽  
Momentum Conservation ◽  
Black Hole Horizon ◽  
De Sitter ◽  
Quantum Tunnelling ◽  
Sitter Background

When a particle with angular momentum tunnels across the event horizon of Schwarzschild–de Sitter black hole, the black hole will change into a Kerr–de Sitter one. Considering Hawking radiation as a process of quantum tunnelling near a black-hole horizon, the emission rate of the particles with angular momentum is calculated under energy and angular momentum conservation, and the result is consistent with an underlying unitary theory.PACS Nos.: 97.60.Lf, 04.70.Dy, 03.65.Pm

scholarly journals Black Hole as a Quantum Field Configuration

Universe ◽  
2020 ◽  
Vol 6 (6) ◽  
pp. 77
Author(s):  
Hikaru Kawai ◽  
Yuki Yokokura
Keyword(s):  
Black Hole ◽  
Total Energy ◽  
Hawking Radiation ◽  
Energy Flow ◽  
Scalar Fields ◽  
Back Reaction ◽  
Quantum Field ◽  
S Waves ◽  
Self Consistent ◽  
Matter Fields

We describe 4D evaporating black holes as quantum field configurations by solving the semi-classical Einstein equation G μ ν = 8 π G ⟨ ψ | T μ ν | ψ ⟩ and quantum matter fields in a self-consistent manner. As the matter fields, we consider N massless free scalar fields (N is large). We find a spherically symmetric self-consistent solution of the metric g μ ν and the state | ψ ⟩ . Here, g μ ν is locally A d S 2 × S 2 geometry, and | ψ ⟩ provides ⟨ ψ | T μ ν | ψ ⟩ = ⟨ 0 | T μ ν | 0 ⟩ + T μ ν ( ψ ) , where | 0 ⟩ is the ground state of the matter fields in the metric and T μ ν ( ψ ) consists of the excitation of s-waves that describe the collapsing matter and Hawking radiation with the ingoing negative energy flow. This object is supported by a large tangential pressure ⟨ 0 | T θ θ | 0 ⟩ due to the vacuum fluctuation of the bound modes with large angular momenta l ≫ 1 . This describes the interior of the black hole when the back reaction of the evaporation is taken into account. In this picture, the black hole is a compact object with a surface (instead of horizon) that looks like a conventional black hole from the outside and eventually evaporates without a singularity. If we count the number of configurations { | ψ ⟩ } that satisfy the self-consistent equation, we reproduce the area law of the entropy. This tells that the information is carried by the s-waves inside the black hole. | ψ ⟩ also describes the process that the negative ingoing energy flow created with Hawking radiation is superposed on the collapsing matter to decrease the total energy while the total energy density remains positive. Finally, as a special case, we consider conformal matter fields and show that the interior metric is determined by the matter content of the theory, which leads to a new constraint to the matter contents for the black hole to evaporate.

BLACK HOLES HAVE LONG HAIR

2012 ◽  
Vol 21 (11) ◽  
pp. 1242003 ◽  
Author(s):  
SHAHAR HOD
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Spatial Behavior ◽  
Black Hole Horizon ◽  
Hairy Black Holes ◽  
Matter Fields ◽  
Circular Geodesic ◽  
Hairy Black Hole

The influential "no-hair" conjecture suggests that black holes may be characterized by only three conserved parameters: mass, charge and angular momentum. However, counterexamples in which the conjecture fails are well-known in the literature. In this essay we study such Einstein-matter theories in which hairy black-hole configurations have been discovered. In particular, we analyze the spatial behavior of the matter fields which reside outside the black-hole horizon. We prove a theorem which reveals the central role played by the null circular geodesic (the "photonsphere") of such hairy black holes. According to this theorem, the asymptotic decline of the hair outside the horizon cannot start before the black-hole photonsphere is crossed. We therefore conclude that hairy black holes must have long hair which extends beyond the photonsphere.

scholarly journals Maxwell–Boltzmann type Hawking radiation

2017 ◽  
Vol 32 (12) ◽  
pp. 1750071 ◽  
Author(s):  
Youngsub Yoon
Keyword(s):  
Black Hole ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Boltzmann Distribution ◽  
Black Hole Horizon ◽  
Not Given ◽  
Horizon Area ◽  
Einstein Distribution ◽  
Bose Einstein

Twenty years ago, Rovelli proposed that the degeneracy of black hole (i.e. the exponential of the Bekenstein–Hawking entropy) is given by the number of ways the black hole horizon area can be expressed as a sum of unit areas. However, when counting the sum, one should treat the area quanta on the black hole horizon as distinguishable. This distinguishability of area quanta is noted in Rovelli’s paper. Building on this idea, we derive that the Hawking radiation spectrum is not given by Planck radiation spectrum (i.e. Bose–Einstein distribution) but given by Maxwell–Boltzmann distribution.

scholarly journals PROMOTING FINITE TO INFINITE SYMMETRIES: THE (3 + 1)-DIMENSIONAL ANALOGUE OF THE VIRASORO ALGEBRA AND HIGHER-SPIN FIELDS

2000 ◽  
Vol 15 (14) ◽  
pp. 939-944 ◽  
Author(s):  
M. CALIXTO
Keyword(s):  
Gauge Theories ◽  
Conformal Symmetry ◽  
Virasoro Algebra ◽  
De Sitter ◽  
Infinite Dimensional ◽  
Higher Spin ◽  
Spin Fields ◽  
Conformal Gauge ◽  
Matter Fields ◽  
Integrable Field

Infinite enlargements of finite pseudo-unitary symmetries are explicitly provided in this letter. The particular case of u (2, 2) ≃ so (4, 2) ⊕ u (1) constitutes a (Virasoro-like) infinite-dimensional generalization of the (3 + 1) -dimensional conformal symmetry, in addition to matter fields with all conformal spins. These algebras provide a new arena for integrable field models in higher dimensions; for example, anti-de Sitter and conformal gauge theories of higher-so(4, 2)-spin fields. A proposal for a noncommutative geometrical interpretation of space is also outlined.

scholarly journals COMBINING THE TUNNELING AND ANOMALY PHENOMENA IN DERIVING THE GRAVITATIONAL ANOMALY

2009 ◽  
Vol 24 (32) ◽  
pp. 2639-2648 ◽  
Author(s):  
SUBIR GHOSH
Keyword(s):  
Black Hole ◽  
Energy Level ◽  
Hawking Radiation ◽  
Black Hole Physics ◽  
Negative Energy ◽  
Conformal Anomaly ◽  
Spectral Flow ◽  
Gravitational Anomaly ◽  
Zero Energy ◽  
Dirac Sea

In the present work we have derived the gravitational anomaly from a fundamentally different perspective: it emerges due to the tunneling of particles (in the present case fermions) across the black hole horizon. The latter effect is in fact the Hawking radiation. We have used the analogy of an early idea17,18 of visualizing chiral gauge anomaly as an effect of spectral flow of the energy levels, from the negative energy Dirac sea, across zero energy level in the presence of gauge interactions. This was extended to conformal anomaly in Ref. 23. In the present work, we exploit the latter formalism in black hole physics where we interpret crossing the horizon of black hole (the zero energy level) as a spectral flow since it is also accompanied by a change of sign in the energy of the particle. Furthermore, Hawking radiation induces a shrinking of the radius of the horizon15,16 which reminds us of a similar rearrangement in the Fermi level generated by the spectral flow.17,18,21 Hence in our formulation the negative energy states below horizon play a similar role as the Dirac sea. We successfully recover the gravitational anomaly.

GROUND STATES UNDER GRAVITY AND BLACK HOLE EVAPORATION

1991 ◽  
Vol 06 (15) ◽  
pp. 1341-1346
Author(s):  
KENJI FUKAZAWA
Keyword(s):  
Black Hole ◽  
Shell Model ◽  
Ground State ◽  
Hawking Radiation ◽  
Particle Creation ◽  
Point Of View ◽  
Spatial Infinity ◽  
Black Hole Evaporation ◽  
State Of Matter ◽  
Matter Fields

One may expect that the ground state of matter fields depends on the strength of gravity on account of the particle creation by the effect of gravity. In this letter we examine the argument of Hawking from this point of view by considering the shell model. We find that an observer at rest at spatial infinity can ‘see’ no radiation while an observer at rest near the horizon ‘sees’ Hawking radiation. Note that the latter thinks that the radiation is to be ‘seen’ at spatial infinity.

Fluctuation on a Schwarzschild black hole

2009 ◽  
Vol 87 (9) ◽  
pp. 1009-1012 ◽  
Author(s):  
Xianming Liu ◽  
Wenbiao Liu
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Hawking Radiation ◽  
Apparent Horizon ◽  
Gravitational Anomaly ◽  
Schwarzschild Black Hole ◽  
First Law Of Thermodynamics ◽  
Vaidya Black Hole

When a relativistic perturbation is given to the horizon of a Schwarzschild black hole, a new supersurface near the horizon will be obtained. Using the gravitational anomaly method proposed by Robinson and Wilczek, Hawking radiation from this new supersurface is calculated. It is found that the first law of thermodynamics can also be constructed successfully on this supersurface. The expressions of the characteristic position and temperature are very similar to the previous results for the event horizon of a Vaidya black hole. Comparing with the Vaidya black hole, we conclude that Hawking radiation and the thermodynamics of a Vaidya black hole should be indeed constructed at the apparent horizon instead of the event horizon.

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