Shadows of boson and Proca stars with thin accretion disks
In this work, we obtain the shadow images of spherically symmetric scalar boson and Proca stars using analytical fittings of numerical solutions, when illuminated by a geometrically thin accretion disk. We chose a sample of four boson and four Proca stars with radii ranging from more compact configu...
| Autores: | ; |
|---|---|
| Tipo de documento: | Artículo |
| Fecha de publicación: | 2022 |
| País: | España |
| Institución: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Lenguaje: | Inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/72792 |
| Acceso en línea: | https://hdl.handle.net/20.500.14352/72792 |
| Nivel de acceso: | Acceso abierto |
| Palabra clave: | 51-73 Black hole Física-Modelos matemáticos Física matemática |
| _version_ | 1878730202717093888 |
|---|---|
| author | Rosa, Joao Luis |
| author2 | Rubiera García, Diego |
| author2_role | author |
| author_browse | Rosa, Joao Luis Rubiera García, Diego |
| author_facet | Rosa, Joao Luis Rubiera García, Diego |
| author_role | author |
| collection | Docta Complutense |
| description | In this work, we obtain the shadow images of spherically symmetric scalar boson and Proca stars using analytical fittings of numerical solutions, when illuminated by a geometrically thin accretion disk. We chose a sample of four boson and four Proca stars with radii ranging from more compact configurations with R '' 9M to more dilute configurations with R '' 20M, where M is the total mass of the bosonic star. In these configurations, the absence of the light sphere (the locus of unstable bound geodesics) makes the optical appearance of these stars to be dominated by a single luminous ring enclosing a central brightness depression, and no further photon rings are available. We show that if one considers face-on observations and a disk model whose emission is truncated at some finite radius at which the luminosity attains its maximum value, both the size of the shadow, as well as the luminosity and depth of the bright region, are heavily influenced by the emission profile, with the choice of the type and parameters of the bosonic stars in our samples having a sub-dominant influence. These differences are nonetheless significantly magnified when one allows the accretion disk to extend close enough to the center of the star. Our results point out that even though bosonic stars are horizonless and do not have a photon sphere, some of them may be able to produce conventional black hole shadowlike images provided that their compactness is large enough, thus being potentially consistent with current and future observations. |
| eu_rights_str_mv | openAccess |
| format | article |
| id | ES_179009f1f6bb0b707a8a39b0fb29a4c7 |
| institution | Universidad Complutense de Madrid (UCM) |
| instname_str | Universidad Complutense de Madrid (UCM) |
| language | eng |
| network_acronym_str | ES |
| network_name_str | España |
| oai_identifier_str | oai:docta.ucm.es:20.500.14352/72792 |
| publishDate | 2022 |
| publishDateSort | 2022 |
| publisher | Amer Physical Soc |
| publisherStr | Amer Physical Soc |
| reponame_str | Docta Complutense |
| spelling | Shadows of boson and Proca stars with thin accretion disks Rosa, Joao Luis Rubiera García, Diego 51-73 Black hole Física-Modelos matemáticos Física matemática In this work, we obtain the shadow images of spherically symmetric scalar boson and Proca stars using analytical fittings of numerical solutions, when illuminated by a geometrically thin accretion disk. We chose a sample of four boson and four Proca stars with radii ranging from more compact configurations with R '' 9M to more dilute configurations with R '' 20M, where M is the total mass of the bosonic star. In these configurations, the absence of the light sphere (the locus of unstable bound geodesics) makes the optical appearance of these stars to be dominated by a single luminous ring enclosing a central brightness depression, and no further photon rings are available. We show that if one considers face-on observations and a disk model whose emission is truncated at some finite radius at which the luminosity attains its maximum value, both the size of the shadow, as well as the luminosity and depth of the bright region, are heavily influenced by the emission profile, with the choice of the type and parameters of the bosonic stars in our samples having a sub-dominant influence. These differences are nonetheless significantly magnified when one allows the accretion disk to extend close enough to the center of the star. Our results point out that even though bosonic stars are horizonless and do not have a photon sphere, some of them may be able to produce conventional black hole shadowlike images provided that their compactness is large enough, thus being potentially consistent with current and future observations. Amer Physical Soc https://hdl.handle.net/20.500.14352/72792 |
| spellingShingle | Shadows of boson and Proca stars with thin accretion disks Rosa, Joao Luis 51-73 Black hole Física-Modelos matemáticos Física matemática |
| title | Shadows of boson and Proca stars with thin accretion disks |
| title_full | Shadows of boson and Proca stars with thin accretion disks |
| title_fullStr | Shadows of boson and Proca stars with thin accretion disks |
| title_full_unstemmed | Shadows of boson and Proca stars with thin accretion disks |
| title_short | Shadows of boson and Proca stars with thin accretion disks |
| title_sort | Shadows of boson and Proca stars with thin accretion disks |
| topic | 51-73 Black hole Física-Modelos matemáticos Física matemática |
| topic_facet | 51-73 Black hole Física-Modelos matemáticos Física matemática |
| url | https://hdl.handle.net/20.500.14352/72792 |