Einstein-Maxwell-scalar black holes: the hot, the cold and the bald

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dc.contributor.authorBlázquez Salcedo, José Luis
dc.contributor.authorHerdeiro, Carlos A.R.
dc.contributor.authorKunz, Jutta
dc.contributor.authorPombo, Alexandre M.
dc.contributor.authorRadu, Eugen
dc.date.accessioned2024-02-05T09:40:41Z
dc.date.available2024-02-05T09:40:41Z
dc.date.issued2020-07-10
dc.description.abstractThe phenomenon of spontaneous scalarisation of charged black holes (BHs) has recently motivated studies of various Einstein-Maxwell-scalar models. Within these models, different classes of BH solutions are possible, depending on the non-minimal coupling function f(φ), between the scalar field and the Maxwell invariant. Here we consider the class wherein both the (bald) electrovacuum Reissner-Nordström (RN) BH and new scalarised BHs co-exist, and the former are never unstable against scalar perturbations. In particular we examine the model, within this subclass, with a quartic coupling function: f(φ) =1 +α(φ)4. The domain of existence of the scalarised BHs, for fixed α, is composed of two branches. The first branch (coldscalarised BHs) is continuously connected to the extremal RN BH. The second branch (hotscalarised BHs) connects to the first one at the minimum value of the charge to mass ratio and it includes overcharged BHs. We then assess the perturbative stability of the scalarised solutions, focusing on spherical perturbations. On the one hand, cold scalarised BHs are shown to be unstable by explicitly computing growing modes. The instability is quenched at both endpoints of the first branch. On the other hand, hot scalarised BHs are shown to be stable by using the S-deformation method. Thus, in the spherical sector this model possesses two stable BH local ground states (RN and hot scalarised). We point out that the branch structure of BHs in this model parallels the one of BHs in five dimensional vacuum gravity, with [Myers-Perry BHs, fat rings, thin rings] playing the role of [RN, cold scalarised, hot scalarised] BHs.
dc.description.departmentDepto. de Física Teórica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipGerman Research Foundation
dc.description.sponsorshipEuropean Cooperation in Science and Technology
dc.description.sponsorshipFundacao para a Ciencia e a Tecnologia
dc.description.sponsorshipEuropean Union's Horizon 2020 Research and Innovation
dc.description.statuspub
dc.identifier.doi10.1016/J.PHYSLETB.2020.135493
dc.identifier.essn1434-6052
dc.identifier.issn1434-6044
dc.identifier.officialurlhttps://www.sciencedirect.com/science/article/pii/S0370269320302975?via%3Dihub
dc.identifier.urihttps://hdl.handle.net/20.500.14352/98719
dc.journal.titlePhysics Letters B
dc.language.isoeng
dc.page.final135493-8
dc.page.initial135493-1
dc.publisherElsevier
dc.relation.projectIDCA15117
dc.relation.projectIDBL 1553
dc.relation.projectIDPD/BD/142842/2018
dc.relation.projectIDUIDB/04106/2020
dc.relation.projectIDUIDP/04106/2020
dc.relation.projectIDFunFiCO-777740
dc.relation.projectIDCA16104
dc.relation.projectIDPTDC/FIS-OUT/28407/2017
dc.relation.projectIDCERN/FIS-PAR/0027/2019
dc.relation.projectIDPTDC/FIS-AST/3041/2020
dc.rightsAttribution 4.0 Internationalen
dc.rights.accessRightsopen access
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/
dc.subject.cdu53
dc.subject.keywordPhysics
dc.subject.ucmFísica (Física)
dc.subject.unesco22 Física
dc.titleEinstein-Maxwell-scalar black holes: the hot, the cold and the bald
dc.typejournal article
dc.type.hasVersionVoR
dc.volume.number806
dspace.entity.typePublication
relation.isAuthorOfPublication2a6d99a8-5cf7-4359-b1e1-b96adfb2fb3f
relation.isAuthorOfPublication.latestForDiscovery2a6d99a8-5cf7-4359-b1e1-b96adfb2fb3f
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