Center of mass energy of the collision for two general geodesic particles around a Kerr-Newman-Taub-NUT black hole

Zakria, Ayesha; Jamil, Mubasher

doi:10.1007/jhep05(2015)147

“…The study of the structure of the spacetime and test particle motion around black holes can be found in Refs. [39][40][41][42][43][44][45][46][47][48][49][50][51]. A number of studies are devoted to study the electromagnetic field and particle motion around black holes in the presence of an external magnetic field .…”

Section: Introductionmentioning

confidence: 99%

Dynamics of test particles around a Bardeen black hole surrounded by perfect fluid dark matter

Narzilloev

¹

,

Rayimbaev

²

,

Shaymatov

³

et al. 2020

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We study the dynamics of (i) neutral test particles, (ii) magnetically charged test particles, and (iii) test magnetic dipole around a regular Bardeen black hole surrounded by perfect fluid dark matter (PFDM). It has been shown how the magnetic charge of the black hole and the parameter of the surrounding PFDM can influence the innermost stable circular orbit (ISCO) radius of a test particle. We have found that the ISCO radius is strongly affected as a consequence of the combined effect of the magnetic charge parameter and the perfect fluid dark matter. The black hole magnetic charge parameter g and the combined effect of perfect fluid dark matter can mimic the black hole rotation parameter up to a/M ≈ 0.9. It has been observed that the ISCO for magnetic dipole disappears at the values exceeding the calculated upper value for the magnetic interaction parameter β. The upper limit decreases with the increase of both the dark matter and magnetic charge parameters. Finally, as an astrophysical application, we have analyzed degeneracy effects of spin of Kerr black holes and magnetic charge of regular Bardeen black holes for the different values of the dark matter parameter providing exactly the same value for ISCO radius of a magnetic dipole with the same value of the parameter β = 10.2 of the magnetar called PSR J1745-2900 orbiting around supermassive black hole Sagittarius A*. It has been observed that the magnetic charge of the pure regular Bardeen black hole can mimic the spin of a Kerr black hole up to a/M 0.8085, while upper limit for the magnetic charge which may provide ISCO for the magnetic dipole is gupper 0.65M . In the presence of PFDM with the parameter α = 0.01(0.05), the upper limit for the magnetic charge decreases and equals to gupper 0.62M (0.548M ) and consequently mimicker value for the spin parameter of black hole lies in the range of a/M ∈ (0.0106 ÷ 0.8231) ( a/M ∈ (0.0816 ÷ 0.8595)). We also show that the same values of the spin of Kerr black hole and the magnetic charge of regular Bardeen black hole surrounded by PFDM provide the same values for the ISCO radius of the chosen magnetar.

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“…To study the spacetime structure around RN black hole one may consider the test particle motion [11][12][13][14][15][16][17][18][19][20][21][22]. The properties of the RN solution and impact of the electromagnetic field on spacetime structure around compact objects have been explored in Refs.…”

Section: Introductionmentioning

confidence: 99%

Distinguishing magnetically and electrically charged Reissner–Nordström black holes by magnetized particle motion

Juraeva

¹

,

Rayimbaev

²

,

Abdujabbarov

³

et al. 2021

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In the present paper, we investigate the dynamics of magnetized particles around magnetically and electrically Reissner–Nordström (RN) black hole. The main idea of the work is to distinguish the effects of electric and magnetic charges of the RN black hole and spin of the rotating Kerr black hole through the dynamics of the magnetized particles. In this study, we have treated a magnetized neutron star as a magnetized test particle, in particular, the magnetar SGR (PSR) J1745-2900 orbiting around the supermassive black hole Sagittarius A* (SMBH SgrA*) with the magnetic interaction parameter $$b=0.716$$ b = 0.716 and the parameter $$\beta =10.2$$ β = 10.2 . The comparison of the effects of the magnetic and electric charges, and magnetic interaction parameters on the dynamics of the magnetar modeled as a magnetized particle near the SMBH Sgr A* has shown that the magnetic charge of the RN black hole can mimic the spin parameter of a rotating Kerr black hole up to $$a/M \simeq 0.82$$ a / M ≃ 0.82 . The external magnetic field can mimic the magnetic charge of the RN black hole up to $$Q_m/M=0.4465$$ Q m / M = 0.4465 . We have shown that the electric charge of the RN black hole can mimic the black hole magnetic charge up to $$Q_m/M=0.5482$$ Q m / M = 0.5482 and the magnetic field interaction with the magnetized particle acts against the increase of the mimicking value of the black hole spin parameter. The studies may be helpful to explain the observability of radio pulsars around the SMBH SgrA* system and taking it as a real astrophysical laboratory to get more precise constraints on the central black hole and dominated parameters of the alternate gravity. Finally, we have investigated the effects of magnetic and electric charge of the RN black hole in the center-of-mass energy of head-on collisions of magnetized particles with neutral, electrically charged, and magnetized particles. Both electric and magnetic charges of the RN black hole would lead to an increase in the center of the mass–energy of the collisions.

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“…The detailed specifications of these changes and test particle motion around compact object in the presence of a magnetic field have been studied in Refs. [48,[82][83][84][85][86][87][88][89][90][91][92][93][94][95][96][97][98][99][100]. The structure of the electromagnetic field around compact objects in alternate and modified theories of gravity has been explored in Refs.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of charged particles and magnetic dipoles around magnetized quasi-Schwarzschild black holes

Narzilloev

¹

,

Rayimbaev

²

,

Abdujabbarov

³

et al. 2021

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In the present paper, we have investigated the motion of charged particles together with magnetic dipoles to determine how well the spacetime deviation parameter $$\epsilon $$ ϵ and external uniform magnetic field can mimic the spin of a rotating Kerr black hole. Investigation of charged particle motion has shown that the deviation parameter $$\epsilon $$ ϵ in the absence of an external magnetic fields can mimic the rotation parameter of the Kerr spacetime up to $$a/M \approx 0.5$$ a / M ≈ 0.5 . The combination of an external magnetic field and deviation parameter can do even a better job mimicking the rotation parameter up to $$a/M\simeq 0.93$$ a / M ≃ 0.93 , which corresponds to the rapidly rotating case. Study of the dynamics of the magnetic dipoles around quasi-Schwarzschild black holes in the external magnetic field has shown that there are degeneracy values of the ISCO radius of test particles at $$\epsilon _{cr}>\epsilon \ge 0.35$$ ϵ cr > ϵ ≥ 0.35 which may lead to two different values of the innermost stable circular orbit (ISCO) radius. When the deviation parameter is in the range of $$\epsilon \in (-1,\ 1)$$ ϵ ∈ ( - 1 , 1 ) , it can mimic the spin of a rotating Kerr black hole in the range $$a/M \in (0.0537, \ 0.3952)$$ a / M ∈ ( 0.0537 , 0.3952 ) for magnetic dipoles with values of the magnetic coupling parameter $$\beta \in [-0.25,\ 0.25]$$ β ∈ [ - 0.25 , 0.25 ] in corotating orbits.

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Center of mass energy of the collision for two general geodesic particles around a Kerr-Newman-Taub-NUT black hole

Cited by 52 publications

References 42 publications

Dynamics of test particles around a Bardeen black hole surrounded by perfect fluid dark matter

Dynamics of test particles around a Bardeen black hole surrounded by perfect fluid dark matter

Distinguishing magnetically and electrically charged Reissner–Nordström black holes by magnetized particle motion

Dynamics of charged particles and magnetic dipoles around magnetized quasi-Schwarzschild black holes

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