Motion of test particles in the field of a naked singularity
We investigate the motion of test particles in the gravitational field of a static naked singularity generated by a mass distribution with a quadrupole moment. We use the quadrupole metric (q metric) which is the simplest generalization of the Schwarzschild metric with a quadrupole parameter. We stu...
- Autores:
- Tipo de recurso:
- Fecha de publicación:
- 2016
- Institución:
- Universidad Tecnológica de Bolívar
- Repositorio:
- Repositorio Institucional UTB
- Idioma:
- eng
- OAI Identifier:
- oai:repositorio.utb.edu.co:20.500.12585/8993
- Acceso en línea:
- https://hdl.handle.net/20.500.12585/8993
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- Rights
- restrictedAccess
- License
- http://creativecommons.org/licenses/by-nc-nd/4.0/
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Motion of test particles in the field of a naked singularity |
| title |
Motion of test particles in the field of a naked singularity |
| spellingShingle |
Motion of test particles in the field of a naked singularity |
| title_short |
Motion of test particles in the field of a naked singularity |
| title_full |
Motion of test particles in the field of a naked singularity |
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Motion of test particles in the field of a naked singularity |
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Motion of test particles in the field of a naked singularity |
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Motion of test particles in the field of a naked singularity |
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We investigate the motion of test particles in the gravitational field of a static naked singularity generated by a mass distribution with a quadrupole moment. We use the quadrupole metric (q metric) which is the simplest generalization of the Schwarzschild metric with a quadrupole parameter. We study the influence of the quadrupole on the motion of massive test particles and photons and show that the behavior of the geodesics can drastically depend on the values of the quadrupole parameter. In particular, we prove explicitly that the perihelion distance depends on the value of the quadrupole. Moreover, we show that an accretion disk on the equatorial plane of the quadrupole source can be either continuous or discrete, depending on the value of the quadrupole. The inner radius of the disk can be used in certain cases to determine the value of the quadrupole parameter. The case of a discrete accretion is interpreted as due to the presence of repulsive gravity generated by the naked singularity. Radial geodesics are also investigated and compared with the Schwarzschild counterparts. © 2016 American Physical Society. |
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2016 |
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2016 |
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2020-03-26T16:32:44Z |
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2020-03-26T16:32:44Z |
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Physical Review D; Vol. 93, Núm. 2 |
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24700010 |
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https://hdl.handle.net/20.500.12585/8993 |
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10.1103/PhysRevD.93.024024 |
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Universidad Tecnológica de Bolívar |
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Repositorio UTB |
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Physical Review D; Vol. 93, Núm. 2 24700010 10.1103/PhysRevD.93.024024 Universidad Tecnológica de Bolívar Repositorio UTB 54883880400 56815070600 25225467000 55989741100 56336189300 |
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https://hdl.handle.net/20.500.12585/8993 |
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eng |
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American Physical Society |
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2020-03-26T16:32:44Z2020-03-26T16:32:44Z2016Physical Review D; Vol. 93, Núm. 224700010https://hdl.handle.net/20.500.12585/899310.1103/PhysRevD.93.024024Universidad Tecnológica de BolívarRepositorio UTB5488388040056815070600252254670005598974110056336189300We investigate the motion of test particles in the gravitational field of a static naked singularity generated by a mass distribution with a quadrupole moment. We use the quadrupole metric (q metric) which is the simplest generalization of the Schwarzschild metric with a quadrupole parameter. We study the influence of the quadrupole on the motion of massive test particles and photons and show that the behavior of the geodesics can drastically depend on the values of the quadrupole parameter. In particular, we prove explicitly that the perihelion distance depends on the value of the quadrupole. Moreover, we show that an accretion disk on the equatorial plane of the quadrupole source can be either continuous or discrete, depending on the value of the quadrupole. The inner radius of the disk can be used in certain cases to determine the value of the quadrupole parameter. The case of a discrete accretion is interpreted as due to the presence of repulsive gravity generated by the naked singularity. Radial geodesics are also investigated and compared with the Schwarzschild counterparts. © 2016 American Physical Society.Recurso electrónicoapplication/pdfengAmerican Physical Societyhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/restrictedAccessAtribución-NoComercial 4.0 Internacionalhttp://purl.org/coar/access_right/c_16echttps://www.scopus.com/inward/record.uri?eid=2-s2.0-84956547300&doi=10.1103%2fPhysRevD.93.024024&partnerID=40&md5=a6e0254f437fe7b52caa8b23a12ef7ffMotion of test particles in the field of a naked singularityinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArtículohttp://purl.org/coar/version/c_970fb48d4fbd8a85http://purl.org/coar/resource_type/c_2df8fbb1Boshkayev K.Gasperín E.Gutiérrez-Piñeres A.C.Quevedo H.Toktarbay S.Kerr, R.P., (1963) Phys. Rev. Lett., 11, p. 237De Felice, F., (1978) Nature (London), 273, p. 429Calvani, M., Nobili, L., (1979) Nuovo Cimento Soc. Ital. Fis. B, 51, p. 247Rudnicki, W., (1998) Acta Phys. Pol., 29, p. 981Penrose, R., (1969) Riv. Nuovo Cimento, 1, p. 252Hawking, S.W., Ellis, G.F.R., (1973) The Large Scale Structure of Space-Time, , (Cambridge University Press, Cambridge, England)Joshi, P.S., (2007) Gravitational Collapse and Spacetime Singularities, , (Cambridge University Press, Cambridge, England)Joshi, P.S., Malafarina, D., Narayan, R., (2014) Classical Quantum Gravity, 31, p. 015002Ortiz Sarbach O, N., Zannias, T., (2015) Classical Quantum Gravity, 32, p. 247001Zipoy, D.M., (1966) J. Math. Phys. (N.Y.), 7, p. 1137Voorhees, B., (1970) Phys. Rev. D, 2, p. 2119Pugliese, D., Quevedo, H., Ruffini, R., (2011) Phys. Rev. D, 83, p. 024021Pugliese, D., Quevedo, H., Ruffini, R., (2011) Phys. Rev. D, 83, p. 104052Stephani, H., Kramer, D., MacCallum, M.A.H., Hoenselaers, C., Herlt, E., (2003) Exact Solutions of Einstein's Field Equations, , (Cambridge University Press, Cambridge, England)Quevedo, H., (2011) Gen. Relativ. Gravit., 43, p. 1141Quevedo, H., (1990) Fortschr. Phys., 38, p. 733Quevedo, H., (2011) Int. J. Mod. Phys. D, 20, p. 1779Malafarina, D., (2004) Conf. Proc., C0405132, p. 273Wald, R., (1984) General Relativity, , (University of Chicago Press, Chicago)Tod, P., (2011) Gen. Relativ. Gravit., 43, p. 1855Geroch, R., (1970) J. Math. Phys. (N.Y.), 11, p. 1955Geroch, R., (1970) J. Math. Phys. (N.Y.), 11, p. 2580Parnovsky, S., (1985) Zh. Eksp. Teor. Fiz., 88, p. 1921Parnovsky, S., (1985) JETP, 61, p. 1139Papadopoulos, D., Stewart, B., Witten, L., (1981) Phys. Rev. D, 24, p. 320Herrera, L., Hernandez-Pastora, J.L., (2000) J. Math. Phys. (N.Y.), 41, p. 7544Herrera, L., Magli, G., Malafarina, D., (2005) Gen. Relativ. Gravit., 37, p. 1371Dadhich, N., Date, G., arXiv:gr-qc/0012093Kodama, H., Hikida, W., (2003) Classical Quantum Gravity, 20, p. 5121Chowdhury, A.N., Patil, M., Malafarina, D., Joshi, P.S., (2012) Phys. Rev. D, 85, p. 104031Quevedo, H., Parkes, L., (1989) Gen. Relativ. Gravit., 21, p. 1047Pugliese, D., Quevedo, H., Ruffini, R., (2013) Phys. Rev. D, 88, p. 024042Pugliese, D., Quevedo, H., (2015) Eur. Phys. J. C, 75, p. 234Luongo, O., Quevedo, H., Toward an invariant definition of repulsive gravity (2012) Proceedings of the Twelfth Marcel Grossmann Meeting on General Relativity, p. 1029. , edited by T. Damour, R. T. Jantzen, and R. Ruffini (World Scientific, Singapore), Part B, p.Luongo, O., Quevedo, H., arXiv:1005.4532Luongo, O., Quevedo, H., (2014) Phys. Rev. D, 90, p. 084032Toktarbay, S., Quevedo, H., (2014) Gravitation and Cosmology, 20, p. 252http://purl.org/coar/resource_type/c_6501THUMBNAILMiniProdInv.pngMiniProdInv.pngimage/png23941https://repositorio.utb.edu.co/bitstream/20.500.12585/8993/1/MiniProdInv.png0cb0f101a8d16897fb46fc914d3d7043MD5120.500.12585/8993oai:repositorio.utb.edu.co:20.500.12585/89932021-02-02 14:18:13.043Repositorio Institucional UTBrepositorioutb@utb.edu.co |