BAKALA, Pavel, Vittorio DE FALCO, Emmanuele BATTISTA, Kateřina GOLUCHOVÁ, Debora LANČOVÁ, Maurizio FALANGA and Luigi STELLA. Three-dimensional general relativistic Poynting-Robertson effect. II. Radiation field from a rigidly rotating spherical source. Physical Review D. 2019, vol. 100, No 10, p. "104053-1"-"104053-20", 20 pp. ISSN 2470-0010. Available from: https://dx.doi.org/10.1103/PhysRevD.100.104053.
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Basic information
Original name Three-dimensional general relativistic Poynting-Robertson effect. II. Radiation field from a rigidly rotating spherical source
Authors BAKALA, Pavel (203 Czech Republic, belonging to the institution), Vittorio DE FALCO (380 Italy, belonging to the institution), Emmanuele BATTISTA (380 Italy, belonging to the institution), Kateřina GOLUCHOVÁ (203 Czech Republic, guarantor, belonging to the institution), Debora LANČOVÁ (203 Czech Republic, belonging to the institution), Maurizio FALANGA (756 Switzerland) and Luigi STELLA (380 Italy).
Edition Physical Review D, 2019, 2470-0010.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United States of America
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19240/19:A0000440
Organization unit Faculty of Philosophy and Science in Opava
Doi http://dx.doi.org/10.1103/PhysRevD.100.104053
UT WoS 000498879200010
Keywords in English Poynting-Robertson effect;rotating spherical source;trajectories of test particles;compact objects
Tags FÚ, GA17-16287S, RCCPDP, RIVOK, SGS13-2019
Tags International impact, Reviewed
Links GA17-16287S, research and development project.
Changed by Changed by: Jan Vlha, učo 48995. Changed: 27/4/2021 09:40.
Abstract
We investigate the three-dimensional, general relativistic Poynting-Robertson (PR) effect in the case of rigidly rotating spherical source which emits radiation radially in the local comoving frame. Such radiation field is meant to approximate the field produced by the surface of a rotating neutron star, or by the central radiating hot corona of accreting black holes; it extends the purely radial radiation field that we considered in a previous study. Its angular momentum is expressed in terms of the rotation frequency and radius of the emitting source. For the background we adopt a Kerr spacetime geometry. We derive the equations of motion for test particles influenced by such radiation field, recovering the classical and weak-field approximation for slow rotation. We concentrate on solutions consisting of particles orbiting along circular orbits off and parallel to the equatorial plane, which are stabilized by the balance between gravitational attraction, radiation force and PR drag. Such solutions are found to lie on a critical hypersurface, whose shape may morph from prolate to oblate depending on the Kerr spin parameter and the luminosity, rotation and radius of the radiating sphere. For selected parameter ranges, the critical hypersurface intersects the radiating sphere giving rise to a bulging equatorial region or, alternatively, two lobes above the poles. We calculate the trajectories of test particles in the close vicinity of the critical hypersurface for a selected set of initial parameters and analyze the spatial and angular velocity of test particles captured on the critical hypersurface.
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