Black hole pulsar

Levin, Janna; D’Orazio, Daniel J.; García-Sáenz, Sebastián

doi:10.1103/physrevd.98.123002

Cited by 54 publications

(49 citation statements)

References 63 publications

(67 reference statements)

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“…This can be related to the ionization of accretion disk either by decay of infalling neutral particle into charged fragments or due to charge separation in a relativistic plasma of accretion disk. In the latter scenario black hole may behave as a pulsar [56] with net stable charge of both black hole and surrounding magnetosphere with respect to observer at rest at infinity. Ejection of ionized particles to infinity takes place along magnetic field lines, which can be open to infinity at the polar caps of black holes.…”

Section: Discussionmentioning

confidence: 99%

Fifty Years of Energy Extraction from Rotating Black Hole: Revisiting Magnetic Penrose Process

Tursunov

Dadhich

2019

Universe

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Magnetic Penrose process (MPP) is not only the most exciting and fascinating process mining the rotational energy of black hole but it is also the favored astrophysically viable mechanism for high energy sources and phenomena. It operates in three regimes of efficiency, namely low, moderate and ultra, depending on the magnetization and charging of spinning black holes in astrophysical setting. In this paper, we revisit MPP with a comprehensive discussion of its physics in different regimes, and compare its operation with other competing mechanisms. We show that MPP could in principle foot the bill for powering engine of such phenomena as ultra-high-energy cosmic rays, relativistic jets, fast radio bursts, quasars, AGNs, etc. Further, it also leads to a number of important observable predictions. All this beautifully bears out the promise of a new vista of energy powerhouse heralded by Roger Penrose half a century ago through this process, and it has today risen in its magnetically empowered version of mid 1980s from a purely thought experiment of academic interest to a realistic powering mechanism for various high-energy astrophysical phenomena.

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Section: Discussionmentioning

confidence: 99%

Fifty Years of Energy Extraction from Rotating Black Hole: Revisiting Magnetic Penrose Process

Tursunov

Dadhich

2019

Universe

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“…To simplify the set-up, we neglect the BH spin and assume the final BH to be Schwarzschild. (also see [11]) Q ≈ EM 2 ≈ B NS r 2 NS , where M is BH mass and E ∼ (v rel /c)B NS ≈ B NS is the magnitude of the induced electric field. To get an intuition about the BH charge Q, we define a dimensionless quantity…”

mentioning

confidence: 84%

“…The associated electromagnetic emission during the merger mainly originates from the surrounding plasma within the system, which has a much smaller energy reservoir than a typical sGRB. A few mechanisms that might lighten up these systems have been proposed, e.g., DC circuit [9,10], BH pulsar [11] and BH electric generator [12]. Previous discussions focused on estimating the energy budget rather than description about the plasma dynamics and emission properties, so that the spectroscopic prediction of EM counterparts has not been made.…”

mentioning

confidence: 99%

Black hole discharge: Very-high-energy gamma rays from black hole-neutron star mergers

Pan

Yang

2019

Phys. Rev. D

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With mass ratio larger than ∼ 5, star disruption is not expected for a black hole merging with a neutron star during the final plunge phase. In the late inspiral stage, the black hole is likely charged as it cuts through the magnetic field carried by the neutron star, leaving a temporarily charged black hole after merger. The unstable charged state of the remnant black hole rapidly neutralizes by interacting with the surrounding plasma and photons, which we investigate in first principle by numerically solving a coupled set of Boltzmann equations. The resulting basic picture is as follows. Electrons and positrons are accelerated in the BH electric field, which then lose energy to surrounding soft photons via Compton scattering; more electrons and positrons will be created from pair production as the hard photons colliding with soft photons, or through the Schwinger process in strong electromagnetic fields. The cascade stops when the charged black hole accretes enough opposite charges and becomes neutralized. We find that ∼ 10% (which depends on the soft photon energy and number density) of the total electric energy is carried away to infinity in a time interval ∼ 1 ms by very-high-energy (> 50 GeV, the low energy detection threshold of the MAGIC telescope) gamma rays whose spectrum is approximately a power law with spectral index ∼ −2.3.

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“…We use a subscript "NS" to indicate the quantities of an NS (those without subscript "NS" are the BH's). For a spinning BH-magnetized NS binary in an electro-vacuum approximation, as shown in Levin et al (2018), the BH could not only be charged stably but also maintain the Wald's charge quantity Q = Q W until the NS plunges into the BH, even though EM emission during the charging process and continual flux of charges within the BH-NS system occurs. During this plunging period, as the separation between BH and NS reaches the NS's radius (r → R NS ), Wald's maximal charge quantity of the BH is…”

Section: Processes Post a Magnetized Ns Plunging Into A Spinning Bhmentioning

confidence: 99%

Electromagnetic Emission Post Spinning Black Hole Magnetized Neutron Star Mergers

Zhong

Dai

Deng

2019

ApJ

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For a binary composed of a spinning black hole (BH) (with mass 7M ⊙ ) and a strongly magnetized neutron star (NS) (with surface magnetic field strength B S,NS 10 12 G and mass ∼ 1.4M ⊙ ), the NS as a whole will possibly eventually plunge into the BH. During the inspiral phase, the spinning BH could be charged to the Wald charge quantity Q W until merger in an electro-vacuum approximation. During the merger, if the spinning charged BH creates its own magnetosphere due to an electric field strong enough for pair cascades to spark, the charged BH would transit from electro-vacuum to force-free cases and could discharge in a time 1 ms. As the force-free magnetosphere is full of a highly conducting plasma, the magnetic flux over the NS's caps would be retained outside the BH's event horizon under the frozen-in condition. Based on this scenario, we here investigate three possible energy-dissipation mechanisms that could produce electromagnetic (EM) counterparts in a time interval of the BH's discharge post a BH-NS merger-induced gravitational wave event: (1) magnetic reconnection at the BH's poles would occur, leading to a millisecond bright EM signal, (2) a magnetic shock in the zone of closed magnetic field lines due to the detachment and reconnection of the entire BH magnetic field would probably produce a bright radio emission, e.g., a fast radio burst, and (3) the Blandford-Znajek mechanism would extract the BH's rotational energy, giving rise to a millisecond-duration luminous high-energy burst. We also calculate the luminosities due to these mechanisms as a function of BH's spin for different values of B S,NS .

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Black hole pulsar

Cited by 54 publications

References 63 publications

Fifty Years of Energy Extraction from Rotating Black Hole: Revisiting Magnetic Penrose Process

Fifty Years of Energy Extraction from Rotating Black Hole: Revisiting Magnetic Penrose Process

Black hole discharge: Very-high-energy gamma rays from black hole-neutron star mergers

Electromagnetic Emission Post Spinning Black Hole Magnetized Neutron Star Mergers

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