Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole
Autor(a) principal: | |
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Data de Publicação: | 2022 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1103/PhysRevD.106.024047 http://hdl.handle.net/11449/240647 |
Resumo: | We study extreme mass ratio inspirals occurring in modified gravity, for which the system is modeled by a small compact object with scalar charge spiraling into a supermassive Kerr black hole. Besides the tensorial gravitational waves arising from the metric perturbations, radiation is also induced by the scalar field. The relevant metric and scalar perturbations are triggered by the orbital motion of the small object, which give rise to a system of inhomogeneous differential equations under the adiabatic approximation. Such a system of equations is then solved numerically using a Green's function furnished by the solutions of the corresponding homogeneous equations. To explore the present scenario from an observational perspective, we investigate how the pertinent observables are dependent on specific spacetime configurations. In this regard, the energy fluxes and the gravitational-wave dephasing accumulated during the process are evaluated, as functions of the scalar charge, mass ratio, and spin of the central supermassive black hole. In particular, the presence of additional scalar emission leads to a more significant rate of overall energy loss which, in turn, decreases the total number of orbital cycles before the small object plunges into the central black hole. Moreover, for a central black hole with a higher spin, the imprints of the scalar charge on the resultant gravitational radiation are found to be more significant, which indicates the possibility of detecting the scalar charge. |
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Detection of scalar fields by extreme mass ratio inspirals with a Kerr black holeWe study extreme mass ratio inspirals occurring in modified gravity, for which the system is modeled by a small compact object with scalar charge spiraling into a supermassive Kerr black hole. Besides the tensorial gravitational waves arising from the metric perturbations, radiation is also induced by the scalar field. The relevant metric and scalar perturbations are triggered by the orbital motion of the small object, which give rise to a system of inhomogeneous differential equations under the adiabatic approximation. Such a system of equations is then solved numerically using a Green's function furnished by the solutions of the corresponding homogeneous equations. To explore the present scenario from an observational perspective, we investigate how the pertinent observables are dependent on specific spacetime configurations. In this regard, the energy fluxes and the gravitational-wave dephasing accumulated during the process are evaluated, as functions of the scalar charge, mass ratio, and spin of the central supermassive black hole. In particular, the presence of additional scalar emission leads to a more significant rate of overall energy loss which, in turn, decreases the total number of orbital cycles before the small object plunges into the central black hole. Moreover, for a central black hole with a higher spin, the imprints of the scalar charge on the resultant gravitational radiation are found to be more significant, which indicates the possibility of detecting the scalar charge.Center for Gravitation and Cosmology College of Physical Science and Technology Yangzhou UniversityShanghai Frontier Research Center for Gravitational Wave Detection Shanghai Jiao Tong UniversitySchool of Aeronautics and Astronautics Shanghai Jiao Tong UniversitySchool of Physics Huazhong University of Science and Technology, HubeiEscola de Engenharia de Lorena Universidade de São Paulo, SPFaculdade de Engenharia de Guaratinguetá Universidade Estadual Paulista, Guaratinguetá, SPFaculdade de Engenharia de Guaratinguetá Universidade Estadual Paulista, Guaratinguetá, SPYangzhou UniversityShanghai Jiao Tong UniversityHuazhong University of Science and TechnologyUniversidade de São Paulo (USP)Universidade Estadual Paulista (UNESP)Guo, HongLiu, YunqiZhang, ChaoGong, YunguiQian, Wei-Liang [UNESP]Yue, Rui-Hong2023-03-01T20:26:38Z2023-03-01T20:26:38Z2022-07-15info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.1103/PhysRevD.106.024047Physical Review D, v. 106, n. 2, 2022.2470-00292470-0010http://hdl.handle.net/11449/24064710.1103/PhysRevD.106.0240472-s2.0-85135939936Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengPhysical Review Dinfo:eu-repo/semantics/openAccess2023-03-01T20:26:38Zoai:repositorio.unesp.br:11449/240647Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462023-03-01T20:26:38Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
title |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
spellingShingle |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole Guo, Hong |
title_short |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
title_full |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
title_fullStr |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
title_full_unstemmed |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
title_sort |
Detection of scalar fields by extreme mass ratio inspirals with a Kerr black hole |
author |
Guo, Hong |
author_facet |
Guo, Hong Liu, Yunqi Zhang, Chao Gong, Yungui Qian, Wei-Liang [UNESP] Yue, Rui-Hong |
author_role |
author |
author2 |
Liu, Yunqi Zhang, Chao Gong, Yungui Qian, Wei-Liang [UNESP] Yue, Rui-Hong |
author2_role |
author author author author author |
dc.contributor.none.fl_str_mv |
Yangzhou University Shanghai Jiao Tong University Huazhong University of Science and Technology Universidade de São Paulo (USP) Universidade Estadual Paulista (UNESP) |
dc.contributor.author.fl_str_mv |
Guo, Hong Liu, Yunqi Zhang, Chao Gong, Yungui Qian, Wei-Liang [UNESP] Yue, Rui-Hong |
description |
We study extreme mass ratio inspirals occurring in modified gravity, for which the system is modeled by a small compact object with scalar charge spiraling into a supermassive Kerr black hole. Besides the tensorial gravitational waves arising from the metric perturbations, radiation is also induced by the scalar field. The relevant metric and scalar perturbations are triggered by the orbital motion of the small object, which give rise to a system of inhomogeneous differential equations under the adiabatic approximation. Such a system of equations is then solved numerically using a Green's function furnished by the solutions of the corresponding homogeneous equations. To explore the present scenario from an observational perspective, we investigate how the pertinent observables are dependent on specific spacetime configurations. In this regard, the energy fluxes and the gravitational-wave dephasing accumulated during the process are evaluated, as functions of the scalar charge, mass ratio, and spin of the central supermassive black hole. In particular, the presence of additional scalar emission leads to a more significant rate of overall energy loss which, in turn, decreases the total number of orbital cycles before the small object plunges into the central black hole. Moreover, for a central black hole with a higher spin, the imprints of the scalar charge on the resultant gravitational radiation are found to be more significant, which indicates the possibility of detecting the scalar charge. |
publishDate |
2022 |
dc.date.none.fl_str_mv |
2022-07-15 2023-03-01T20:26:38Z 2023-03-01T20:26:38Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://dx.doi.org/10.1103/PhysRevD.106.024047 Physical Review D, v. 106, n. 2, 2022. 2470-0029 2470-0010 http://hdl.handle.net/11449/240647 10.1103/PhysRevD.106.024047 2-s2.0-85135939936 |
url |
http://dx.doi.org/10.1103/PhysRevD.106.024047 http://hdl.handle.net/11449/240647 |
identifier_str_mv |
Physical Review D, v. 106, n. 2, 2022. 2470-0029 2470-0010 10.1103/PhysRevD.106.024047 2-s2.0-85135939936 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Physical Review D |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
_version_ |
1803649772392808448 |