Feebly interacting dark matter particle as the inflaton

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dc.contributor University of Helsinki, Department of Physics en
dc.contributor.author Tenkanen, Tommi
dc.date.accessioned 2017-01-27T15:11:01Z
dc.date.available 2017-01-27T15:11:01Z
dc.date.issued 2016-09
dc.identifier.citation Tenkanen , T 2016 , ' Feebly interacting dark matter particle as the inflaton ' , Journal of High Energy Physics , vol. 2016 , no. 09 , 049 , pp. 49 . https://doi.org/10.1007/JHEP09(2016)049 en
dc.identifier.issn 1029-8479
dc.identifier.other PURE: 78953975
dc.identifier.other PURE UUID: 400ac852-72d7-4e14-b518-3b70cced5af4
dc.identifier.other Bibtex: urn:e09495b293815c1d6ec28da642492e78
dc.identifier.other Scopus: 84986557053
dc.identifier.other WOS: 000411320600001
dc.identifier.uri http://hdl.handle.net/10138/174157
dc.description.abstract We present a scenario where a Z 2-symmetric scalar field ϕ first drives cosmic inflation, then reheats the Universe but remains out-of-equilibrium itself, and finally comprises the observed dark matter abundance, produced by particle decays à la freeze-in mechanism. We work model-independently without specifying the interactions of the scalar field besides its self-interaction coupling, $ϕ 4, non-minimal coupling to gravity, $ϕ 2 R, and coupling to another scalar field, gϕ 2 $ 2. We find the scalar field ϕ serves both as the inflaton and a dark matter candidate if 10−9 ≲ $ ≲ g ≲ 10−7 and 3 keV ≲ m ϕ ≲ 85 MeV for $ = O 1 backslashxi =backslashmathcalO(1) . Such a small value of the non-minimal coupling is also found to be of the right magnitude to produce the observed curvature perturbation amplitude within the scenario. We also discuss how the model may be distinguished from other inflationary models of the same type by the next generation CMB satellites. en
dc.format.extent 14
dc.language.iso eng
dc.relation.ispartof Journal of High Energy Physics
dc.rights en
dc.subject 114 Physical sciences en
dc.title Feebly interacting dark matter particle as the inflaton en
dc.type Article
dc.description.version Peer reviewed
dc.identifier.doi https://doi.org/10.1007/JHEP09(2016)049
dc.type.uri info:eu-repo/semantics/other
dc.type.uri info:eu-repo/semantics/publishedVersion
dc.contributor.pbl
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