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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.typeresearch article
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.type.publicationarticle
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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