Signatures of Dark Matter Burning in Nuclear Star Clusters
Autor(a) principal: | |
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Data de Publicação: | 2011 |
Outros Autores: | |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
Texto Completo: | http://hdl.handle.net/10174/3886 https://doi.org/10.1088/2041-8205/733/2/L51 |
Resumo: | In order to characterize how dark matter (DM) annihilation inside stars changes the aspect of a stellar cluster, we computed the evolution until the ignition of the He burning of stars from 0.7 M sun to 3.5 M sun within halos of DM with different characteristics. We found that, when a cluster is surrounded by a dense DM halo, the positions of the cluster' stars in the H-R diagram have a brighter and hotter turnoff point than in the classical scenario without DM, therefore giving the cluster a younger appearance. The high DM densities required to produce these effects are expected only in very specific locations, such as near the center of our Galaxy. In particular, if DM is formed by the 8 GeV weakly interacting massive particles recently invoked to reconcile the results from direct detection experiments, then this signature is predicted for halos of DM with a density ρχ = 3 × 105 GeV cm-3. A DM density gradient inside the stellar cluster would result in a broader main sequence, turnoff, and red giant branch regions. Moreover, we found that for very high DM halo densities the bottom of the isochrones in the H-R diagram rises to higher luminosities, leading to a characteristic signature on the stellar cluster. We argue that this signature could be used to indirectly probe the presence of DM particles in the location of a cluster. |
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Signatures of Dark Matter Burning in Nuclear Star ClustersAstrophysicsAstronomyIn order to characterize how dark matter (DM) annihilation inside stars changes the aspect of a stellar cluster, we computed the evolution until the ignition of the He burning of stars from 0.7 M sun to 3.5 M sun within halos of DM with different characteristics. We found that, when a cluster is surrounded by a dense DM halo, the positions of the cluster' stars in the H-R diagram have a brighter and hotter turnoff point than in the classical scenario without DM, therefore giving the cluster a younger appearance. The high DM densities required to produce these effects are expected only in very specific locations, such as near the center of our Galaxy. In particular, if DM is formed by the 8 GeV weakly interacting massive particles recently invoked to reconcile the results from direct detection experiments, then this signature is predicted for halos of DM with a density ρχ = 3 × 105 GeV cm-3. A DM density gradient inside the stellar cluster would result in a broader main sequence, turnoff, and red giant branch regions. Moreover, we found that for very high DM halo densities the bottom of the isochrones in the H-R diagram rises to higher luminosities, leading to a characteristic signature on the stellar cluster. We argue that this signature could be used to indirectly probe the presence of DM particles in the location of a cluster.2012-01-19T16:20:23Z2012-01-192011-06-01T00:00:00Zinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://hdl.handle.net/10174/3886http://hdl.handle.net/10174/3886https://doi.org/10.1088/2041-8205/733/2/L51engilopes@uevora.ptnd343Lopes, IlidioCasanellas, Jordiinfo: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:RCAAP2024-01-03T18:41:25Zoai:dspace.uevora.pt:10174/3886Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T00:59:16.229295Repositório 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 |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
title |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
spellingShingle |
Signatures of Dark Matter Burning in Nuclear Star Clusters Lopes, Ilidio Astrophysics Astronomy |
title_short |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
title_full |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
title_fullStr |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
title_full_unstemmed |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
title_sort |
Signatures of Dark Matter Burning in Nuclear Star Clusters |
author |
Lopes, Ilidio |
author_facet |
Lopes, Ilidio Casanellas, Jordi |
author_role |
author |
author2 |
Casanellas, Jordi |
author2_role |
author |
dc.contributor.author.fl_str_mv |
Lopes, Ilidio Casanellas, Jordi |
dc.subject.por.fl_str_mv |
Astrophysics Astronomy |
topic |
Astrophysics Astronomy |
description |
In order to characterize how dark matter (DM) annihilation inside stars changes the aspect of a stellar cluster, we computed the evolution until the ignition of the He burning of stars from 0.7 M sun to 3.5 M sun within halos of DM with different characteristics. We found that, when a cluster is surrounded by a dense DM halo, the positions of the cluster' stars in the H-R diagram have a brighter and hotter turnoff point than in the classical scenario without DM, therefore giving the cluster a younger appearance. The high DM densities required to produce these effects are expected only in very specific locations, such as near the center of our Galaxy. In particular, if DM is formed by the 8 GeV weakly interacting massive particles recently invoked to reconcile the results from direct detection experiments, then this signature is predicted for halos of DM with a density ρχ = 3 × 105 GeV cm-3. A DM density gradient inside the stellar cluster would result in a broader main sequence, turnoff, and red giant branch regions. Moreover, we found that for very high DM halo densities the bottom of the isochrones in the H-R diagram rises to higher luminosities, leading to a characteristic signature on the stellar cluster. We argue that this signature could be used to indirectly probe the presence of DM particles in the location of a cluster. |
publishDate |
2011 |
dc.date.none.fl_str_mv |
2011-06-01T00:00:00Z 2012-01-19T16:20:23Z 2012-01-19 |
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://hdl.handle.net/10174/3886 http://hdl.handle.net/10174/3886 https://doi.org/10.1088/2041-8205/733/2/L51 |
url |
http://hdl.handle.net/10174/3886 https://doi.org/10.1088/2041-8205/733/2/L51 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
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ilopes@uevora.pt nd 343 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
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openAccess |
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reponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação instacron:RCAAP |
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Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação |
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RCAAP |
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RCAAP |
reponame_str |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
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Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
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Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação |
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