Reheating constraints to Palatini Coleman-Weinberg inflation

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dc.authorid0000-0002-1129-4345
dc.contributor.authorBostan, Nilay
dc.date.accessioned2024-07-31T09:07:35Z
dc.date.available2024-07-31T09:07:35Z
dc.date.issued2024-02-21
dc.departmentTENMAK-Nükleer Enerji Araştırma Enstitüsü-Ankara
dc.description.abstractIn this work, we examine the reheating constraints to symmetry-breaking mechanism, which is associated with Coleman-Weinberg inflation in the early universe. We consider the Coleman-Weinberg inflation potential,wheretheinflatonhasa v ̸= 0 afterinflation. Setting Treh = 105 GeV,wefirstshow wreh dependency on ns, r, and N∗ for AV case. Then, we demonstrate the results of ns, r, N∗, α = dns/dlnk for different reheating temperatures and compare the results with the latest BICEP/Keck data. We also present that ns−r and ns−N∗ planes and the effect of reheating temperature which is in a wide range, on inflationary predictions for both AV and BV cases. Finally, we indicate how N∗ and α change according to the reheating temperature values.
dc.identifier.doi10.55730/1300-0101.2754
dc.identifier.eissn1303-6122
dc.identifier.endpage39
dc.identifier.startpage28
dc.identifier.urihttps://kurumsalarsiv.tenmak.gov.tr/handle/20.500.12878/2018
dc.identifier.volume48
dc.institutionauthorBostan, Nilay
dc.language.isoen
dc.publisherTübitak
dc.relation.journalTurkish Journal of Physics
dc.relation.publicationcategoryMakale- Ulusal- Editör Deneyimli Dergi
dc.rightsinfo:eu-repo/semantics/openAccess
dc.subjectCosmology
dc.subjectinflation
dc.subjectreheating
dc.titleReheating constraints to Palatini Coleman-Weinberg inflation
dc.typearticle
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