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dc.contributor.authorHertzberg, Mark P.
dc.contributor.authorNurmi, Sami
dc.contributor.authorSchiappacasse, Enrico D.
dc.contributor.authorYanagida, Tsutomu T.
dc.date.accessioned2021-03-30T05:03:52Z
dc.date.available2021-03-30T05:03:52Z
dc.date.issued2021
dc.identifier.citationHertzberg, M. P., Nurmi, S., Schiappacasse, E. D., & Yanagida, T. T. (2021). Shining primordial black holes. <i>Physical Review D</i>, <i>103</i>(6), Article 063025. <a href="https://doi.org/10.1103/PhysRevD.103.063025" target="_blank">https://doi.org/10.1103/PhysRevD.103.063025</a>
dc.identifier.otherCONVID_52593999
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/74882
dc.description.abstractWe study the well-motivated mixed dark matter (DM) scenario composed of a dominant thermal WIMP, highlighting the case of SU(2)L triplet fermion “winos,” with a small fraction of primordial black holes (PBHs). After the wino kinetic decoupling, the DM particles are captured by PBHs leading to the presence of PBHs with dark minihalos in the Milky Way today. The strongest constraints for the wino DM come from the production of narrow line gamma rays from wino annihilation in the Galactic Center. We analyse in detail the viability of the mixed wino DM scenario, and determine the constraints on the fraction of DM in PBHs assuming a cored halo profile in the Milky Way. We show that already with the sensitivity of current indirect searches, there is a significant probability for detecting a gamma ray signal characteristic for the wino annihilation in a single nearby dressed PBH when MPBH∼M⊙, which we refer to as a “shining black hole.” Similar results should apply also in more general setups with ultracompact minihalos or other DM models, since the accretion of DM around large overdensities and DM annihilation are both quite generic processes.en
dc.format.mimetypeapplication/pdf
dc.languageeng
dc.language.isoeng
dc.publisherAmerican Physical Society
dc.relation.ispartofseriesPhysical Review D
dc.rightsCC BY 4.0
dc.titleShining primordial black holes
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-202103302214
dc.contributor.laitosFysiikan laitosfi
dc.contributor.laitosDepartment of Physicsen
dc.type.urihttp://purl.org/eprint/type/JournalArticle
dc.description.reviewstatuspeerReviewed
dc.relation.issn2470-0010
dc.relation.numberinseries6
dc.relation.volume103
dc.type.versionpublishedVersion
dc.rights.copyright© 2021 the Authors
dc.rights.accesslevelopenAccessfi
dc.relation.grantnumber318319
dc.subject.ysomustat aukot
dc.subject.ysokosmologia
dc.subject.ysopimeä aine
dc.subject.ysoastrofysiikka
dc.format.contentfulltext
jyx.subject.urihttp://www.yso.fi/onto/yso/p18360
jyx.subject.urihttp://www.yso.fi/onto/yso/p7160
jyx.subject.urihttp://www.yso.fi/onto/yso/p14101
jyx.subject.urihttp://www.yso.fi/onto/yso/p20188
dc.rights.urlhttps://creativecommons.org/licenses/by/4.0/
dc.relation.doi10.1103/PhysRevD.103.063025
dc.relation.funderSuomen Akatemiafi
dc.relation.funderAcademy of Finlanden
jyx.fundingprogramAkatemiahanke, SAfi
jyx.fundingprogramAcademy Project, AoFen
jyx.fundinginformationThis work was supported by the Academy of Finland Grant No. 318319. T. T. Y. is supported in part by the China Grant for Talent Scientific Start-Up Project and the JSPS Grant-in-Aid for Scientific Research Grants No. 16H02176, No. 17H02878, and No. 19H05810 and by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. M. P. H. is supported in part by National Science Foundation Grant No. PHY-2013953.


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