PUGLIESE, Daniela and Hernando QUEVEDO. The ergoregion in the Kerr spacetime: properties of the equatorial circular motion. The European Physical Journal C. US - Spojené státy americké, 2015, vol. 75, No 5, p. "234-1"-"234-20", 20 pp. ISSN 1434-6044. Available from: https://dx.doi.org/10.1140/epjc/s10052-015-3455-0.
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Basic information
Original name The ergoregion in the Kerr spacetime: properties of the equatorial circular motion
Name (in English) The ergoregion in the Kerr spacetime: properties of the equatorial circular motion
Authors PUGLIESE, Daniela and Hernando QUEVEDO.
Edition The European Physical Journal C, US - Spojené státy americké, 2015, 1434-6044.
Other information
Type of outcome Article in a journal
Field of Study 10303 Particles and field physics
Confidentiality degree is not subject to a state or trade secret
WWW URL
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1140/epjc/s10052-015-3455-0
UT WoS 000355681400002
Keywords in English Kerr spacetime; ergoregion; circular geodesic
Tags
Tags International impact, Reviewed
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 30/3/2021 09:05.
Abstract
We investigate in detail the circular motion of test particles in the equatorial plane of the ergoregion in the Kerr spacetime. We consider all the regions where circular motion is allowed, and we analyze the stability properties and the energy and angular momentum of the test particles. We show that the structure of the stability regions has definite features that make it possible to distinguish between black holes and naked singularities. The naked singularity case presents a very structured non-connected set of regions of orbital stability, where the presence of counterrotating particles and zero angular momentum particles for a specific class of naked singularities is interpreted as due to the presence of a repulsive field generated by the centralsource of gravity. In particular, we analyze the effects of the dynamical structure of the ergoregion (the union of the orbital regions for different attractor spins) on the behavior of accretion disks around the central source. The prope
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