Perturbation Method for Classical Spinning Particle Motion: I. Kerr Space-Time

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dc.creatorSingh, Dinesh
dc.date2008-08-22
dc.date2008-10-07
dc.date.accessioned2026-07-07T12:15:18Z
dc.date.available2026-07-07T12:15:18Z
dc.descriptionThis paper presents an analytic perturbation approach to the dynamics of a classical spinning particle, according to the Mathisson-Papapetrou-Dixon (MPD) equations of motion, with a direct application to circular motion around a Kerr black hole. The formalism is established in terms of a power series expansion with respect to the particle's spin magnitude, where the particle's kinematic and dynamical degrees are expressed in a completely general form that can be constructed to infinite order in the expansion parameter. It is further shown that the particle's squared mass and spin magnitude can shift due to a classical analogue of radiative corrections that arise from spin-curvature coupling. Explicit expressions are determined for the case of circular motion near the event horizon a Kerr black hole, where the mass and spin shift contributions are dependent on the initial conditions of the particle's spin orientation. A preliminary analysis of the stability properties of the orbital motion in the Kerr background due to spin-curvature interactions is explored and briefly discussed.
dc.description23 pages; REVTeX file; 9 figures; Accepted for publication in Phys. Rev. D
dc.identifierhttps://arxiv.org/abs/0808.3005
dc.identifierhttp://arxiv.org/abs/0808.3005
dc.identifierPhys.Rev.D78:104028,2008
dc.identifierdoi:10.1103/PhysRevD.78.104028
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/211462
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titlePerturbation Method for Classical Spinning Particle Motion: I. Kerr Space-Time
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