Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star
A full-relativistic approach is used to compute the radius of the innermost stable circular orbit (ISCO), the Keplerian, frame-dragging, precession and oscillation frequencies of the radial and vertical motions of neutral test particles orbiting the equatorial plane of a magnetized neutron star. The...
- Autores:
- Tipo de recurso:
- article
- Fecha de publicación:
- 2013
- Institución:
- Pontificia Universidad Javeriana
- Repositorio:
- Repositorio Universidad Javeriana
- Idioma:
- eng
- OAI Identifier:
- oai:repository.javeriana.edu.co:10554/31274
- Acceso en línea:
- http://revistas.javeriana.edu.co/index.php/scientarium/article/view/5582
http://hdl.handle.net/10554/31274
- Palabra clave:
- Physics
Relativistic precession frequencies; Innermost stable circular orbits; Neutron stars.
null
- Rights
- openAccess
- License
- Atribución-NoComercial-SinDerivadas 4.0 Internacional
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Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron starGutiérrez-Ruiz, Andrés F.; Universidad de AntioquiaPachón, Leonardo A.; Universidad de AntioquiaValenzuela-Toledo, César A.; Universidad del VallePhysicsRelativistic precession frequencies; Innermost stable circular orbits; Neutron stars.nullA full-relativistic approach is used to compute the radius of the innermost stable circular orbit (ISCO), the Keplerian, frame-dragging, precession and oscillation frequencies of the radial and vertical motions of neutral test particles orbiting the equatorial plane of a magnetized neutron star. The space-time around the star is modelled by the six parametric solution derived by Pachón et al. (2012). It is shown that the inclusion of an intense magnetic field, such as the one of a neutron star, have non-negligible effects on the above physical quantities, and therefore, its inclusion is necessary in order to obtain a more accurate and realistic description of physical processes, such as the dynamics of accretion disks, occurring in the neighbourhood of this kind of objects. The results discussed here also suggest that the consideration of strong magnetic fields may introduce non-negligible corrections in, e.g., the relativistic precession model and therefore on the predictions made on the mass of neutron stars.Pontificia Universidad JaverianaFundación para la Promoción de la Investigación y la Tecnología del Banco la República2018-02-24T15:59:32Z2020-04-15T18:10:26Z2018-02-24T15:59:32Z2020-04-15T18:10:26Z2013-12-23http://purl.org/coar/version/c_970fb48d4fbd8a85Artículo de revistahttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionPDFapplication/pdfhttp://revistas.javeriana.edu.co/index.php/scientarium/article/view/558210.11144/Javeriana.SC19-1.isco2027-13520122-7483http://hdl.handle.net/10554/31274enghttp://revistas.javeriana.edu.co/index.php/scientarium/article/view/5582/5860http://revistas.javeriana.edu.co/index.php/scientarium/article/downloadSuppFile/5582/1462Universitas Scientiarum; Vol 19, No 1 (2014); 63-73Universitas Scientiarum; Vol 19, No 1 (2014); 63-73Universitas Scientiarum; Vol 19, No 1 (2014); 63-73nullnullnullAtribución-NoComercial-SinDerivadas 4.0 Internacionalinfo:eu-repo/semantics/openAccesshttp://purl.org/coar/access_right/c_abf2reponame:Repositorio Universidad Javerianainstname:Pontificia Universidad Javerianainstacron:Pontificia Universidad Javeriana2023-03-28T21:15:58Z |
dc.title.none.fl_str_mv |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
title |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
spellingShingle |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star Gutiérrez-Ruiz, Andrés F.; Universidad de Antioquia Physics Relativistic precession frequencies; Innermost stable circular orbits; Neutron stars. null |
title_short |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
title_full |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
title_fullStr |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
title_full_unstemmed |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
title_sort |
Innermost stable circular orbits and epicyclic frequencies around a magnetized neutron star |
dc.creator.none.fl_str_mv |
Gutiérrez-Ruiz, Andrés F.; Universidad de Antioquia Pachón, Leonardo A.; Universidad de Antioquia Valenzuela-Toledo, César A.; Universidad del Valle |
author |
Gutiérrez-Ruiz, Andrés F.; Universidad de Antioquia |
author_facet |
Gutiérrez-Ruiz, Andrés F.; Universidad de Antioquia Pachón, Leonardo A.; Universidad de Antioquia Valenzuela-Toledo, César A.; Universidad del Valle |
author_role |
author |
author2 |
Pachón, Leonardo A.; Universidad de Antioquia Valenzuela-Toledo, César A.; Universidad del Valle |
author2_role |
author author |
dc.contributor.none.fl_str_mv |
Fundación para la Promoción de la Investigación y la Tecnología del Banco la República |
dc.subject.none.fl_str_mv |
Physics Relativistic precession frequencies; Innermost stable circular orbits; Neutron stars. null |
topic |
Physics Relativistic precession frequencies; Innermost stable circular orbits; Neutron stars. null |
description |
A full-relativistic approach is used to compute the radius of the innermost stable circular orbit (ISCO), the Keplerian, frame-dragging, precession and oscillation frequencies of the radial and vertical motions of neutral test particles orbiting the equatorial plane of a magnetized neutron star. The space-time around the star is modelled by the six parametric solution derived by Pachón et al. (2012). It is shown that the inclusion of an intense magnetic field, such as the one of a neutron star, have non-negligible effects on the above physical quantities, and therefore, its inclusion is necessary in order to obtain a more accurate and realistic description of physical processes, such as the dynamics of accretion disks, occurring in the neighbourhood of this kind of objects. The results discussed here also suggest that the consideration of strong magnetic fields may introduce non-negligible corrections in, e.g., the relativistic precession model and therefore on the predictions made on the mass of neutron stars. |
publishDate |
2013 |
dc.date.none.fl_str_mv |
2013-12-23 2018-02-24T15:59:32Z 2018-02-24T15:59:32Z 2020-04-15T18:10:26Z 2020-04-15T18:10:26Z |
dc.type.none.fl_str_mv |
http://purl.org/coar/version/c_970fb48d4fbd8a85 Artículo de revista http://purl.org/coar/resource_type/c_6501 info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://revistas.javeriana.edu.co/index.php/scientarium/article/view/5582 10.11144/Javeriana.SC19-1.isco 2027-1352 0122-7483 http://hdl.handle.net/10554/31274 |
url |
http://revistas.javeriana.edu.co/index.php/scientarium/article/view/5582 http://hdl.handle.net/10554/31274 |
identifier_str_mv |
10.11144/Javeriana.SC19-1.isco 2027-1352 0122-7483 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
http://revistas.javeriana.edu.co/index.php/scientarium/article/view/5582/5860 http://revistas.javeriana.edu.co/index.php/scientarium/article/downloadSuppFile/5582/1462 Universitas Scientiarum; Vol 19, No 1 (2014); 63-73 Universitas Scientiarum; Vol 19, No 1 (2014); 63-73 Universitas Scientiarum; Vol 19, No 1 (2014); 63-73 |
dc.rights.none.fl_str_mv |
Atribución-NoComercial-SinDerivadas 4.0 Internacional info:eu-repo/semantics/openAccess http://purl.org/coar/access_right/c_abf2 |
rights_invalid_str_mv |
Atribución-NoComercial-SinDerivadas 4.0 Internacional http://purl.org/coar/access_right/c_abf2 |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
PDF application/pdf |
dc.coverage.none.fl_str_mv |
null null null |
dc.publisher.none.fl_str_mv |
Pontificia Universidad Javeriana |
publisher.none.fl_str_mv |
Pontificia Universidad Javeriana |
dc.source.none.fl_str_mv |
reponame:Repositorio Universidad Javeriana instname:Pontificia Universidad Javeriana instacron:Pontificia Universidad Javeriana |
instname_str |
Pontificia Universidad Javeriana |
instacron_str |
Pontificia Universidad Javeriana |
institution |
Pontificia Universidad Javeriana |
reponame_str |
Repositorio Universidad Javeriana |
collection |
Repositorio Universidad Javeriana |
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1803712879022571520 |