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dc.contributor.authorEnckell, Vera-Maria
dc.contributor.authorNurmi, Sami
dc.contributor.authorRäsänen, Syksy
dc.contributor.authorTomberg, Eemeli
dc.date.accessioned2021-04-16T10:56:42Z
dc.date.available2021-04-16T10:56:42Z
dc.date.issued2021
dc.identifier.citationEnckell, V.-M., Nurmi, S., Räsänen, S., & Tomberg, E. (2021). Critical point Higgs inflation in the Palatini formulation. <i>Journal of High Energy Physics</i>, <i>2021</i>(4), Article 59. <a href="https://doi.org/10.1007/jhep04(2021)059" target="_blank">https://doi.org/10.1007/jhep04(2021)059</a>
dc.identifier.otherCONVID_66432764
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/75089
dc.description.abstractWe study Higgs inflation in the Palatini formulation with the renormalisation group improved potential in the case when loop corrections generate a feature similar to an inflection point. Assuming that there is a threshold correction for the Higgs quartic coupling λ and the top Yukawa coupling yt, we scan the three-dimensional parameter space formed by the two jumps and the non-minimal coupling ξ. The spectral index ns can take any value in the observationally allowed range. The lower limit for the running is αs > −3.5 × 10−3, and αs can be as large as the observational upper limit. Running of the running is small. The tensor-to-scalar ratio is 2.2×10−17 < r < 2 × 10−5. We find that slow-roll can be violated near the feature, and a possible period of ultra-slow-roll contributes to the widening of the range of CMB predictions. Nevertheless, for the simplest tree-level action, the Palatini formulation remains distinguishable from the metric formulation even when quantum corrections are taken into account, because of the small tensor-to-scalar ratio.en
dc.format.mimetypeapplication/pdf
dc.languageeng
dc.language.isoeng
dc.publisherSpringer
dc.relation.ispartofseriesJournal of High Energy Physics
dc.rightsCC BY 4.0
dc.subject.othercosmology of theories beyond the SM
dc.subject.otherrenormalization group
dc.titleCritical point Higgs inflation in the Palatini formulation
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-202104162394
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.issn1126-6708
dc.relation.numberinseries4
dc.relation.volume2021
dc.type.versionpublishedVersion
dc.rights.copyright© The Authors. Article funded by SCOAP3
dc.rights.accesslevelopenAccessfi
dc.subject.ysoteoreettinen fysiikka
dc.subject.ysokosmologia
dc.format.contentfulltext
jyx.subject.urihttp://www.yso.fi/onto/yso/p38202
jyx.subject.urihttp://www.yso.fi/onto/yso/p7160
dc.rights.urlhttps://creativecommons.org/licenses/by/4.0/
dc.relation.doi10.1007/jhep04(2021)059
dc.type.okmA1


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