Highly relativistic circular orbits of spinning particle in the Kerr field

Plyatsko, Roman; Fenyk, Mykola

doi:10.1103/physrevd.87.044019

Cited by 41 publications

(54 citation statements)

References 65 publications

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“…Another drawback is that the position coordinate obeys a third-order differential equation [2,19]. Nevertheless, since the derivation of the MP equations, they have been applied in different scenarios of general relativity including Schwarzschild and Kerr backgrounds, gravitational waves [20][21][22][23] etc. Influence of a curved background on the motion of a gyroscope allows one to test general relativity in a laboratory (nuclear spin gyroscope measurements of the Earth rotation [24]) or orbital experiments (Probe B experiment).…”

Section: Jhep03(2014)109mentioning

confidence: 99%

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Frenkel electron and a spinning body in a curved background

Ramírez

Дериглазов

Pupasov-Maksimov

2014

J. High Energ. Phys.

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We develop a variational formulation of a particle with spin in a curved spacetime background. The model is based on a singular Lagrangian which provides equations of motion, a fixed value of spin and Frenkel condition on spin-tensor. Comparing our equations with those of Papapetrou we conclude that the Frenkel electron in a gravitational field has the same behavior as a rotating body in the pole-dipole and leading-spin approximation. Due to constraints presented in the formulation, position space is endowed with a noncommutative structure induced by the spin of the particle. Therefore, the model provides a physically interesting example of a noncommutative particle in a curved background.

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Section: Jhep03(2014)109mentioning

confidence: 99%

“…(4.5) usually imposed by hand in the study of a test-body motion in general relativity in pole-dipole approximation [20][21][22][23]. In our approach this condition is embedded into the model from the beginning.…”

Section: Jhep03(2014)109mentioning

confidence: 99%

Frenkel electron and a spinning body in a curved background

Ramírez

Дериглазов

Pupasov-Maksimov

2014

J. High Energ. Phys.

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“…-for details, see [11]. Similarly, the characteristic orbits of spinning particles in non-rotating and rotating axially symmetric space-times, are shifted inward or outward depending on signature of the spin of the particle, with respect to the non-spinning case [20][21][22][23][24][25][26][27][28][29][30][31][32].…”

Section: Introductionmentioning

confidence: 99%

Spinning test particles in the γ spacetime

Toshmatov

Malafarina

2019

Phys. Rev. D

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We consider the motion of spinning particles in the field of a well known vacuum static axially-symmetric space-time, known as γ-metric, that can be interpreted as a generalization of the Schwarzschild manifold to include prolate or oblate deformations. We derive the equations of motion for spinning test particles by using the Mathisson-Papapetrou-Dixon equations together with the Tulczyjew spin-supplementary condition, and restricting the motion to the equatorial plane. We determine the limit imposed by super-luminal velocity for the spin of the particle located at the innermost stable circular orbits (ISCO). We show that the particles on ISCO of the prolate γ space-time are allowed to have higher spin than the corresponding ones in the the oblate case. We determine the value of the ISCO radius depending on the signature of the spin-angular momentum, s − L relation, and show that the value of the ISCO with respect to the non spinning case is bigger for sL < 0 and smaller for sL > 0. The results may be relevant for determining the properties of accretion disks and constraining the allowed values of quadrupole moments of astrophysical black hole candidates.

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“…For extreme Kerr black hole in case of orbital corotation (see (29)), the efficiency is: It means that in case when particle spin is parallel to the total angular momentum of particle and the black hole spins, the efficiency can be larger than 42 %. Note that the ISCO radius and angular frequency do not depend on spin in the case of extreme Kerr BH.…”

Section: Binding Energy In the Innermost Stable Circular Orbitmentioning

confidence: 99%

Parameters of innermost stable circular orbits of spinning test particles: Numerical and analytical calculations

2016

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The motion of classical spinning test particles in the equatorial plane of a Kerr black hole is considered for the case where the particle spin is perpendicular to the equatorial plane. We review some results of our recent research of the innermost stable circular orbits (ISCO) [1] and present some new calculations. The ISCO radius, total angular momentum, energy, and orbital angular frequency are considered. We calculate the ISCO parameters numerically for different values of the Kerr parameter a and investigate their dependence on both black hole and test particle spins. Then we describe in details how to calculate analytically small-spin corrections to the ISCO parameters for an arbitrary values of a. The cases of Schwarzschild, slowly rotating Kerr and extreme Kerr black hole are considered. The use of the orbital angular momentum is discussed. We also consider the ISCO binding energy. It is shown that the efficiency of accretion onto an extreme Kerr black hole can be larger than the maximum known efficiency (42 %) if the test body has a spin.

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Highly relativistic circular orbits of spinning particle in the Kerr field

Cited by 41 publications

References 65 publications

Frenkel electron and a spinning body in a curved background

Frenkel electron and a spinning body in a curved background

Spinning test particles in the γ spacetime

Parameters of innermost stable circular orbits of spinning test particles: Numerical and analytical calculations

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