High efficiency of collisional Penrose process requires heavy particle production

Ogasawara, Kota; Harada, Tomohiro; Miyamoto, Umpei

doi:10.1103/physrevd.93.044054

Cited by 22 publications

(30 citation statements)

References 18 publications

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“…This fact does not necessarily mean the unbounded energy extraction from the black hole, as the particle escaping to the infinity wastes its energy to run up the deep gravitational potential. Nevertheless, some works consistently show that fine-tuned parameters of the particles result in the energy output about 14 times larger than the input energy [6][7][8][9][10][11]. It is worthwhile to notice that the same conclusion is derived even though the deformation of the event horizon caused by energetic particles swallowed by the black hole is taken into account in accordance with the hoop conjecture [12].…”

Section: Introductionsupporting

confidence: 54%

Non-linear collisional Penrose process: How much energy can a black hole release?

Nakao

Okawa

Maeda

2018

Progress of Theoretical and Experimental Physics

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Energy extraction from a rotating or charged black hole is one of fascinating issues in general relativity. The collisional Penrose process is one of such extraction mechanisms and has been reconsidered intensively since Bañados, Silk and West pointed out the physical importance of very high energy collisions around a maximally rotating black hole. In order to get results analytically, the test particle approximation has been adopted so far. Successive works based on this approximation scheme have not yet revealed the upper bound on the efficiency of the energy extraction because of lack of the back reaction. In the Reissner-Nordström spacetime, by fully taking into account the self-gravity of the shells, we find that there is an upper bound on the extracted energy, which is consistent with the area law of a black hole. We also show one particular scenario in which the almost maximum energy extraction is achieved even without the Bañados-Silk-West collision.

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Section: Introductionsupporting

confidence: 54%

Non-linear collisional Penrose process: How much energy can a black hole release?

Nakao

Okawa

Maeda

2018

Progress of Theoretical and Experimental Physics

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“…Creations after the BSW collision near the event horizon are strongly red-shifted and the escape fraction can be diminished [20]. On the other hand, the BSW collision stimulates to reconsider the details of a collisional Penrose process which is a process of extraction of energy from a rotating Kerr black hole after a particle collision [21][22][23][24][25][26][27][28][29][30].…”

Section: Introductionmentioning

confidence: 99%

Particle collision with an arbitrarily high center-of-mass energy near a Bañados-Teitelboim-Zanelli black hole

2017

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We consider a particle collision with a high center-of-mass energy near a Bañados-TeitelboimZanelli (BTZ) black hole. We obtain the center-of-mass energy of two general colliding geodesic particles in the BTZ black hole spacetime. We show that the center-of-mass energy of two ingoing particles can be arbitrarily large on an event horizon if either of the two particles has a critical angular momentum and the other has a non-critical angular momentum. We also show that the motion of a particle with a subcritical angular momentum is allowed near an extremal rotating BTZ black hole and that a center-of-mass energy for a tail-on collision at a point can be arbitrarily large in a critical angular momentum limit.

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“…In particular, the maximum efficiency of the energy extraction becomes possible even without heavy produced particles that are necessary in the Kerr case [22].…”

Section: Quarks-2016mentioning

confidence: 99%

“…Quite recently, the estimates of the efficiency of the energy extraction from the Kerr black hole found in [16] numerically were derived analytically for the Kerr metric [21], [22]. General approach was developed in [23].…”

Section: Quarks-2016mentioning

confidence: 99%

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High energy particle collisions near black holes

Заславский

2016

EPJ Web Conf.

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Abstract. If two geodesic particles collide near a rotating black hole, their energy in the centre of mass frame E c.m. can become unbound under certain conditions (the so-called BSW effect). The special role is played here by so-called critical geodesics when one of particles has fine-tuned energy and angular momentum. The nature of geodesics reveals itself also in fate of the debris after collisions. One of particles moving to a remote observer is necessarily near-critical. We discuss, when such a collision can give rise not only unboud E c.m. but also unbound Killing energy E (so-called super-Penrose process).Investigation of high energy collisions of particles near black holes comes back to works [1] - [3]. In recent years, an interest to this issue revived after the observation made by Bañados, Silk and West (the BSW effect, after the names of its authors) that particle collision near the Kerr black hole can lead, under certain additional conditions, to the unbounded growth of the energy in their centre of mass E c.m. [4]. Later on, in a large series of works, this observation was generalized and extended to other objects and scenarios. The energy that appears in the BSW effect is relevant for an observer who is present just near the point of collision in the vicinity of the black hole horizon. Meanwhile, what is especially physically important is the Killing energy E of debris after such a collision measured by an observer at infinity. Strong redshift "eats" significant part of E c.m. , so it was not quite clear in advance, to what extent the energy E may be high. If E exceeds the initial energy of particles, we are faced with the energy extraction from a black hole. This is a so-called collisional Penrose process (the Penrose process that occurs due to particle collisions). Thus there are two related but different issues: (i) investigation of the effect of unbounded E c.m. , (ii) study of properties of E and the question about the maximum possible efficiency of the collisional Penrose process.Consider the generic axially symmetric metric. It can be written asHere, the metric coefficients do not depend on t and φ. On the horizon N = 0. Alternatively, one can use coordinates θ and r, similar to Boyer-Lindquist ones for the Kerr metric, instead of l and z. In (1) we assume that the metric coefficients are even functions of z, so the equatorial plane θ = π 2 (z = 0) is a symmetry one.In the space-time under discussion there are two conserved quantities u 0 ≡ −E and u φ ≡ L where u μ = dx μ dτ is the four-velocity of a test particle, τ is the proper time and x μ = (t, φ, l, z) are coordinates..The aforementioned conserved quantities have the physical meaning of the energy per unit mass (or frequency for a lightlike particle) and azimuthal component of the angular momentum,

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High efficiency of collisional Penrose process requires heavy particle production

Cited by 22 publications

References 18 publications

Non-linear collisional Penrose process: How much energy can a black hole release?

Non-linear collisional Penrose process: How much energy can a black hole release?

Particle collision with an arbitrarily high center-of-mass energy near a Bañados-Teitelboim-Zanelli black hole

High energy particle collisions near black holes

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