Shadows of Kerr Black Holes with Scalar Hair

Detalhes bibliográficos
Autor(a) principal: Cunha, Pedro V. P.
Data de Publicação: 2015
Outros Autores: Herdeiro, Carlos A. R., Radu, Eugen, Runarsson, Helgi F.
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)
Texto Completo: http://hdl.handle.net/10773/15029
Resumo: Using backwards ray tracing, we study the shadows of Kerr black holes with scalar hair (KBHSH). KBHSH interpolate continuously between Kerr BHs and boson stars (BSs), so we start by investigating the lensing of light due to BSs. Moving from the weak to the strong gravity region, BSs-which by themselves have no shadows-are classified, according to the lensing produced, as (i) noncompact, which yield not multiple images, (ii) compact, which produce an increasing number of Einstein rings and multiple images of the whole celestial sphere, and (iii) ultracompact, which possess light rings, yielding an infinite number of images with (we conjecture) a self-similar structure. The shadows of KBHSH, for Kerr-like horizons and noncompact BS-like hair, are analogous to, but distinguishable from, those of comparable Kerr BHs. But for non-Kerr-like horizons and ultracompact BS-like hair, the shadows of KBHSH are drastically different: novel shapes arise, sizes are considerably smaller, and multiple shadows of a single BH become possible. Thus, KBHSH provide quantitatively and qualitatively new templates for ongoing (and future) very large baseline interferometry observations of BH shadows, such as those of the Event Horizon Telescope.
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spelling Shadows of Kerr Black Holes with Scalar HairUsing backwards ray tracing, we study the shadows of Kerr black holes with scalar hair (KBHSH). KBHSH interpolate continuously between Kerr BHs and boson stars (BSs), so we start by investigating the lensing of light due to BSs. Moving from the weak to the strong gravity region, BSs-which by themselves have no shadows-are classified, according to the lensing produced, as (i) noncompact, which yield not multiple images, (ii) compact, which produce an increasing number of Einstein rings and multiple images of the whole celestial sphere, and (iii) ultracompact, which possess light rings, yielding an infinite number of images with (we conjecture) a self-similar structure. The shadows of KBHSH, for Kerr-like horizons and noncompact BS-like hair, are analogous to, but distinguishable from, those of comparable Kerr BHs. But for non-Kerr-like horizons and ultracompact BS-like hair, the shadows of KBHSH are drastically different: novel shapes arise, sizes are considerably smaller, and multiple shadows of a single BH become possible. Thus, KBHSH provide quantitatively and qualitatively new templates for ongoing (and future) very large baseline interferometry observations of BH shadows, such as those of the Event Horizon Telescope.American Physical Society2016-01-11T12:32:24Z2015-11-16T00:00:00Z2015-11-16info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10773/15029eng0031-900710.1103/PhysRevLett.115.211102Cunha, Pedro V. P.Herdeiro, Carlos A. R.Radu, EugenRunarsson, Helgi F.info:eu-repo/semantics/openAccessreponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãoinstacron:RCAAP2024-02-22T11:27:40Zoai:ria.ua.pt:10773/15029Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T02:50:27.903714Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãofalse
dc.title.none.fl_str_mv Shadows of Kerr Black Holes with Scalar Hair
title Shadows of Kerr Black Holes with Scalar Hair
spellingShingle Shadows of Kerr Black Holes with Scalar Hair
Cunha, Pedro V. P.
title_short Shadows of Kerr Black Holes with Scalar Hair
title_full Shadows of Kerr Black Holes with Scalar Hair
title_fullStr Shadows of Kerr Black Holes with Scalar Hair
title_full_unstemmed Shadows of Kerr Black Holes with Scalar Hair
title_sort Shadows of Kerr Black Holes with Scalar Hair
author Cunha, Pedro V. P.
author_facet Cunha, Pedro V. P.
Herdeiro, Carlos A. R.
Radu, Eugen
Runarsson, Helgi F.
author_role author
author2 Herdeiro, Carlos A. R.
Radu, Eugen
Runarsson, Helgi F.
author2_role author
author
author
dc.contributor.author.fl_str_mv Cunha, Pedro V. P.
Herdeiro, Carlos A. R.
Radu, Eugen
Runarsson, Helgi F.
description Using backwards ray tracing, we study the shadows of Kerr black holes with scalar hair (KBHSH). KBHSH interpolate continuously between Kerr BHs and boson stars (BSs), so we start by investigating the lensing of light due to BSs. Moving from the weak to the strong gravity region, BSs-which by themselves have no shadows-are classified, according to the lensing produced, as (i) noncompact, which yield not multiple images, (ii) compact, which produce an increasing number of Einstein rings and multiple images of the whole celestial sphere, and (iii) ultracompact, which possess light rings, yielding an infinite number of images with (we conjecture) a self-similar structure. The shadows of KBHSH, for Kerr-like horizons and noncompact BS-like hair, are analogous to, but distinguishable from, those of comparable Kerr BHs. But for non-Kerr-like horizons and ultracompact BS-like hair, the shadows of KBHSH are drastically different: novel shapes arise, sizes are considerably smaller, and multiple shadows of a single BH become possible. Thus, KBHSH provide quantitatively and qualitatively new templates for ongoing (and future) very large baseline interferometry observations of BH shadows, such as those of the Event Horizon Telescope.
publishDate 2015
dc.date.none.fl_str_mv 2015-11-16T00:00:00Z
2015-11-16
2016-01-11T12:32:24Z
dc.type.status.fl_str_mv info:eu-repo/semantics/publishedVersion
dc.type.driver.fl_str_mv info:eu-repo/semantics/article
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dc.identifier.uri.fl_str_mv http://hdl.handle.net/10773/15029
url http://hdl.handle.net/10773/15029
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv 0031-9007
10.1103/PhysRevLett.115.211102
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dc.publisher.none.fl_str_mv American Physical Society
publisher.none.fl_str_mv American Physical Society
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