scholarly journals ACCELERATION OF PARTICLES BY QUASIBLACK HOLES

2013 ◽  
Vol 22 (06) ◽  
pp. 1350028 ◽  
Author(s):  
O. B. ZASLAVSKII
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Electric Charge ◽  
Center Of Mass ◽  
Finite Energy ◽  
Fine Tuning ◽  
Black Hole Horizon ◽  
Acceleration Of Particles ◽  
Bsw Effect

If two particles collide near the black hole horizon, the energy in their center of mass (CM) frame can grow indefinitely (the so-called Bañados, Silk and West (BSW) effect). This requires fine-tuning the parameters (the energy–momentum, angular momentum or electric charge) of one particle. We show that the CM energy can be unbound also for collisions in the spacetime of quasiblack holes (QBHs) (the objects on the threshold of forming the horizon which do not collapse). It does not require special fine-tuning of parameters and occurs when any particle inside a QBH having a finite energy collides with the particle that entered a QBH from the outside region.

ACCELERATION OF PARTICLES AS A UNIVERSAL PROPERTY OF ERGOSPHERE

2013 ◽  
Vol 28 (11) ◽  
pp. 1350037 ◽  
Author(s):  
O. B. ZASLAVSKII
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Recent Observation ◽  
Center Of Mass ◽  
Kerr Black Hole ◽  
Acceleration Of Particles ◽  
Axially Symmetric ◽  
Fixed Energy ◽  
Mass Frame

We show that recent observation made by Grib and Pavlov, [A. A. Grib and Yu. V. Pavlov, Europhys. Lett.101, 20004 (2013)] for the Kerr black hole is valid in the general case of rotating axially symmetric metric. Namely, collision of two particles in the ergosphere leads to indefinite growth of the energy in the center-of-mass frame, provided the angular momentum of one of the two particles is negative and increases without limit for a fixed energy at infinity. General approach enabled us to elucidate why the role of the ergosphere is crucial in this process.

scholarly journals Particle Collisions in the Lower Dimensional Rotating Black Hole Space-Time with the Cosmological Constant

2014 ◽  
Vol 2014 ◽  
pp. 1-7 ◽  
Author(s):  
Jie Yang ◽  
Yun-Liang Li ◽  
Yang Li ◽  
Shao-Wen Wei ◽  
Yu-Xiao Liu
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Particle Energy ◽  
Fine Tuning ◽  
Ultrahigh Energy ◽  
Particle Collisions ◽  
Btz Black Hole ◽  
Inner Horizon ◽  
Bsw Effect ◽  
Critical Angular Momentum

We study the effect of ultrahigh energy collisions of two particles with different energies near the horizon of a2+1dimensional BTZ black hole (BSW effect). We find that the particle with the critical angular momentum could exist inside the outer horizon of the BTZ black hole regardless of the particle energy. Therefore, for the nonextremal BTZ black hole, the BSW process is possible on the inner horizon with the fine tuning of parameters which are characterized by the motion of particle, while, for the extremal BTZ black hole, the particle with the critical angular momentum could only exist on the degenerated horizon, and the BSW process could also happen there.

scholarly journals Super-Penrose process due to collisions inside ergosphere

2017 ◽  
Vol 26 (02) ◽  
pp. 1750009
Author(s):  
O. B. Zaslavskii
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Center Of Mass ◽  
Black Hole Horizon ◽  
Mass Frame ◽  
Penrose Process

If two particles collide inside the ergosphere, the energy in the center of mass frame can be made unbound provided at least one of particles has a large negative angular momentum [A. A. Grib and Yu. V. Pavlov, Europhys. Lett. 101 (2013) 20004]. We show that the same condition can give rise to unbounded Killing energy of debris at infinity, i.e. super-Penrose process. Proximity of the point of collision to the black hole horizon is not required.

scholarly journals Infrared effects in the late stages of black hole evaporation

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Éanna É. Flanagan
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Center Of Mass ◽  
Planck Scale ◽  
Black Hole Mass ◽  
Order Unity ◽  
Intrinsic Angular Momentum ◽  
Hole Position ◽  
Late Stages ◽  
Shear Tensor

Abstract As a black hole evaporates, each outgoing Hawking quantum carries away some of the black holes asymptotic charges associated with the extended Bondi-Metzner-Sachs group. These include the Poincaré charges of energy, linear momentum, intrinsic angular momentum, and orbital angular momentum or center-of-mass charge, as well as extensions of these quantities associated with supertranslations and super-Lorentz transformations, namely supermomentum, superspin and super center-of-mass charges (also known as soft hair). Since each emitted quantum has fluctuations that are of order unity, fluctuations in the black hole’s charges grow over the course of the evaporation. We estimate the scale of these fluctuations using a simple model. The results are, in Planck units: (i) The black hole position has a uncertainty of $$ \sim {M}_i^2 $$ ∼ M i 2 at late times, where Mi is the initial mass (previously found by Page). (ii) The black hole mass M has an uncertainty of order the mass M itself at the epoch when M ∼ $$ {M}_i^{2/3} $$ M i 2 / 3 , well before the Planck scale is reached. Correspondingly, the time at which the evaporation ends has an uncertainty of order $$ \sim {M}_i^2 $$ ∼ M i 2 . (iii) The supermomentum and superspin charges are not independent but are determined from the Poincaré charges and the super center-of-mass charges. (iv) The supertranslation that characterizes the super center-of-mass charges has fluctuations at multipole orders l of order unity that are of order unity in Planck units. At large l, there is a power law spectrum of fluctuations that extends up to l ∼ $$ {M}_i^2/M $$ M i 2 / M , beyond which the fluctuations fall off exponentially, with corresponding total rms shear tensor fluctuations ∼ MiM−3/2.

scholarly journals Existence condition and phase transition of Reissner–Nordström–de Sitter black hole

2014 ◽  
Vol 29 (09) ◽  
pp. 1450050 ◽  
Author(s):  
Meng-Sen Ma ◽  
Hui-Hua Zhao ◽  
Li-Chun Zhang ◽  
Ren Zhao
Keyword(s):  
Phase Transition ◽  
Black Hole ◽  
Thermodynamic Properties ◽  
Electric Charge ◽  
Transition Point ◽  
Existence Condition ◽  
Phase Transition Point ◽  
Black Hole Horizon ◽  
Cosmological Horizon ◽  
De Sitter

After introducing the connection between the black hole horizon and the cosmological horizon, we discuss the thermodynamic properties of Reissner–Nordström–de Sitter (RN–dS) space–time. We present the condition under which RN–dS black hole can exist. Employing Ehrenfest' classification, we conclude that the phase transition of RN–dS black hole is the second-order one. The position of the phase transition point is irrelevant to the electric charge of the system. It only depends on the ratio of the black hole horizon and the cosmological horizon.

scholarly journals Angular momentum of an electric charge and magnetically charged black hole

1991 ◽  
Vol 257 (1-2) ◽  
pp. 158-162 ◽  
Author(s):  
David Garfinkle ◽  
Soo-Jong Rey
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Electric Charge ◽  
Charged Black Hole

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 A New Solution of the Einstein-Maxwell Equations for a System with Mass, Magnetic Moment, Charge, and Angular momentum

1974 ◽  
Vol 64 ◽  
pp. 192-192
Author(s):  
Louis Witten
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Magnetic Dipole ◽  
Electric Charge ◽  
Magnetic Moment ◽  
Maxwell Equations ◽  
Black Hole Physics ◽  
Red Shift ◽  
Multipole Moments ◽  
Asymptotically Flat

A five parameter solution of the combined Einstein-Maxwell equations is given which describes a source containing mass, electric charge, magnetic dipole, higher multipole moments of all three kinds, and angular momentum. The solution is asymptotically flat and has a singular infinite red shift surface. Possible relevance of the solution to black hole physics is discussed.

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.

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