Shift of the Isco and Gravitomagnetic Clock Effect Due to Gravitational Spin–orbit Coupling

Shahrear, Pabel; Faruque, Syed Badiuzzaman

doi:10.1142/s0218271807011152

Cited by 8 publications

(8 citation statements)

References 16 publications

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“…The ISCO in different black holes have been investigated in refs. [36][37][38][39][40][41][42][43][44][45]. According to [46], all spherical orbits are not bounded of the black hole.…”

Section: Isco and Mbcomentioning

confidence: 99%

Collision of particles near charged MSW black hole in 2 + 1 dimensions

Saha

Debnath

2019

Mod. Phys. Lett. A

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Here, we explore the dynamics of particle near the horizon of charged Mandal-Sengupta-Wadia (MSW) black hole in 2+1 dimensions. It results analysis of angular momentum and potential energy for null and time-like geodesics. We also appraise the high center-of-mass energy of coming particles from rest at infinity near the horizon of the charged MSW black hole in 2+1 dimension for the extremal case. Finally, we study the ISCO and MBCO radii for this type of black hole. Introduction:Recently, "Two particle collision at the neighborhood of horizons of the black hole" becomes fascinated window in Astrophysics. This method, known as BSW effect, has been firstly achieved by Banados, Silk and West [1] in 2009 for the Kerr black hole to get large center-of-mass (CM) energy if one of particles has critical angular momentum. To get this process, the black hole should be extremal. The CM energy for non-extremal black hole has been demonstrated by Jacobson and Sotiriou [2] where they have pointed out the drawback of this process. So, there must exist astrophysical limitations for extremal Kerr black hole. Lake [3] has found divergent CM energy at inner horizon for rotating Kerr black hole. Liu et al. [4] have studied BSW effect of the Kerr-Taub-NUT space-time for extremal case. Grib and Pavlov [5] have established disbursement of acceleration of the particles to produce high amount of CM energy for a rotating black hole in the case of extremal and non extremal both. Kerr-de Sitter black hole for non extremal case [6] acts as a particle accelerator with unbounded CM energy for two particle collisions. Wei et al. [7] have studied the same thing for the Sen black hole. For non rotating black hole, Zaslavskill [8] has studied particle acceleration. Extension of the BSW effect on particle acceleration on various type of black holes such as charged, non charged, rotating and non rotating black holes have been investigated in [9][10][11][12].Some attractions have been occurred on a new type of black hole, named as Regular black hole with non-singular curvature. Bardeen [13] has introduced First Regular black hole. Then slowly many authors have worked on this type of various black holes in [14][15][16]. Next Amir and Ghosh [17] have studied the rotating Hayward black hole as particle accelerator. Harada [18] has given an excellent review work on particle collision. Several authors have discussed particle collision in [19][20][21]. Now, the lower dimensional setting becomes more sharper than 3+1 dimensional case to get conceptual focus. To solve Einstein gravity equations, 2+1 dimensional black hole is exact solution than 3+1 dimensional black hole. Both 2+ 1 black hole and 3+ 1 black hole contribute same physical *

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“…The ISCO in different black holes have been investigated in refs. [36][37][38][39][40][41][42][43][44][45]. According to [46], all spherical orbits are not bounded of the black hole.…”

Section: Isco and Mbcomentioning

confidence: 99%

Collision of particles near charged MSW black hole in 2 + 1 dimensions

Saha

Debnath

2019

Mod. Phys. Lett. A

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“…Previous to these theoretical advancements, the dynamics of a non-spinning particle moving on a geodesic around a Schwarzschild BH was first studied by Kaplan in [15]. Since then the dynamics of non-spinning particles has been studied vastly by researchers [16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33]. The study of non-spinning particles in the vicinity of different BHs showed that the motion of the massive or massless test particles gets affected by the BHs parameters like mass, charge and rotation.…”

Section: Introductionmentioning

confidence: 99%

Bounds on spinning particles in their innermost stable circular orbits around rotating braneworld black hole

2020

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We study the innermost stable circular orbit (ISCO) of a spinning test particle moving in the vicinity of an axially symmetric rotating braneworld black hole (BH). We start with the description of the event horizon, static limit surface and ergosphere region of such BH and bring out the effect of tidal charge parameter on ergosphere. It is found that the ISCO of rotating braneworld BH is very sensitive to braneworld BH deformation parameter C (also known as tidal charge parameter) in addition to its rotation parameter. We further discovered that the orbital radius of the spinning test particles changes non-monotonously with the braneworld BH deformation parameter. It is found that for rotating braneworld BH the allowed range of the particle spin grows as the tidal charge parameter C decreases, in contrast with the Kerr-Newman BH. We also found the similar behavior of the particle's spin for the braneworld Reissner-Nordström (C < 0) BH in contrast with its general relativity counterpart (i.e., Reissner-Nordström) having (C > 0).

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“…and obtain the differentiate between prograde and retrograde orbits and integrate from zero to 2π. The clock effect is the difference of theses two orbits [8], [9], [10]. The fourth group takes some elements of electromagnetism and does an analogy between Maxwell equations and Einstein linealized equations [11], [12], [13], [14], [15], [16], [17], [18], [19].…”

Section: Introductionmentioning

confidence: 99%

“…and obtain the differentiate between prograde and retrograde orbits and integrate from zero to 2π. The clock effect is the difference of theses two orbits [8], [9], [10].…”

Section: Introductionmentioning

confidence: 99%

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Numerical Solution of Mathisson-Papapetrou-Dixon Equations for Spinning Test Particles in a Kerr Metric

Velandia-Heredia¹,

Tejeiro-Sarmiento²

2018

Momento

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In this work we calculate some estimations of the gravitomagnetic clock effect, taking into consideration not only the rotating gravitational field of the central mass, but also the spin of the test particle, obtaining values for ∆t = t + − t − = 2.5212079035 × 10 −8 s. We use the formulation of Mathisson-Papapetrou-Dixon equations (MPD) for this problem in a Kerr metric. In order to compare our numerical results with previous works, we consider initially only the equatorial plane and also apply the Mathisson-Pirani supplementary spin condition for the spinning test particle. ResumenEn este trabajo nosotros calculamos algunas estimaciones del efecto reloj gravitomagnético, tomando en consideración no sólo el campo rotacional de la masa central, sino también el espín de la partícula de prueba, obteniendo IntroductionIn the last decades, important advances have been made in the study of the gravitomagnetic clock effect. Beginning with the seminal work by Cohen and Mashhoon [1]. In which they presented the influence of the gravitomagnetic field to the proper time of an arbitrary clock about a rotating massive body. In their paper, Cohen and Mashhoon, also showed the possibility of measuring this effect. In this work, we present a theoretical value for the gravitomagnetic clock effect of a spinning test particle orbiting around a rotating massive body. According with the literature, we find different complementary ways that study the phenomena in regard to the gravitomagnetism clock effect. The first way take two family of observers. The first is the family of static observer (or threading observers) with four-velocity m = M −1 ∂ t and world lines along the time coordinate lines. The second famili is the ZAMO's (or slicing observers) with four-velocity n = N −1 ∂ t − N φ ∂ φ and world lines orthogonal to the time coordinate hypersurfaces [2][3][4]. They obtain, in the threading point of view, the local spatial angular direction as

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Shift of the Isco and Gravitomagnetic Clock Effect Due to Gravitational Spin–orbit Coupling

Cited by 8 publications

References 16 publications

Collision of particles near charged MSW black hole in 2 + 1 dimensions

Collision of particles near charged MSW black hole in 2 + 1 dimensions

Bounds on spinning particles in their innermost stable circular orbits around rotating braneworld black hole

Numerical Solution of Mathisson-Papapetrou-Dixon Equations for Spinning Test Particles in a Kerr Metric

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