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dc.contributor.authorAla-Mattinen, Kalle
dc.contributor.authorHeikinheimo, Matti
dc.contributor.authorKainulainen, Kimmo
dc.contributor.authorTuominen, Kimmo
dc.date.accessioned2022-08-15T08:45:25Z
dc.date.available2022-08-15T08:45:25Z
dc.date.issued2022
dc.identifier.citationAla-Mattinen, K., Heikinheimo, M., Kainulainen, K., & Tuominen, K. (2022). Momentum distributions of cosmic relics : Improved analysis. <i>Physical Review D</i>, <i>105</i>(12), Article 123005. <a href="https://doi.org/10.1103/PhysRevD.105.123005" target="_blank">https://doi.org/10.1103/PhysRevD.105.123005</a>
dc.identifier.otherCONVID_150896619
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/82530
dc.description.abstractWe solve coupled momentum-dependent Boltzmann equations for the phase space distribution of cosmic relic particles, without resorting to approximations of assuming kinetic equilibrium or neglecting backscattering or elastic interactions. Our method is amendable to precision numerical computations. To test it, we consider two benchmark models where the momentum dependence of dark matter distribution function is potentially important: a real singlet scalar extension near the Higgs resonance and a sterile neutrino dark matter model with a singlet scalar mediator. The singlet scalar example shows that the kinetic equilibrium may hold surprisingly well even near sharp resonances. However, the integrated method may underestimate the relic density by up to 40% in extreme cases. In the sterile neutrino dark matter model, we studied how the inclusion of previously ignored elastic interactions and processes with initial state sterile neutrinos could affect the nonthermal nature of their resulting distributions. Here the effects turned out to be negligible, proving the robustness of the earlier predictions.en
dc.format.mimetypeapplication/pdf
dc.language.isoeng
dc.publisherAmerican Physical Society (APS)
dc.relation.ispartofseriesPhysical Review D
dc.rightsCC BY 4.0
dc.titleMomentum distributions of cosmic relics : Improved analysis
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-202208154074
dc.contributor.laitosFysiikan laitosfi
dc.contributor.laitosDepartment of Physicsen
dc.type.urihttp://purl.org/eprint/type/JournalArticle
dc.type.coarhttp://purl.org/coar/resource_type/c_2df8fbb1
dc.description.reviewstatuspeerReviewed
dc.relation.issn2470-0010
dc.relation.numberinseries12
dc.relation.volume105
dc.type.versionpublishedVersion
dc.rights.copyright© Authors, 2022
dc.rights.accesslevelopenAccessfi
dc.relation.grantnumber318319
dc.subject.ysokosmologia
dc.subject.ysopimeä aine
dc.subject.ysoneutriinot
dc.format.contentfulltext
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/p5219
dc.rights.urlhttps://creativecommons.org/licenses/by/4.0/
dc.relation.doi10.1103/PhysRevD.105.123005
dc.relation.funderResearch Council of Finlanden
dc.relation.funderSuomen Akatemiafi
jyx.fundingprogramAcademy Project, AoFen
jyx.fundingprogramAkatemiahanke, SAfi
jyx.fundinginformationThis work was supported by the Academy of Finland Grants No. 310130, No. 342777, and No. 318319. K. A.-M. is funded by the doctoral program in Particle Physics and Universe Sciences in University of Helsinki.
dc.type.okmA1


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