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dc.contributor.authorHiçyılmaz, Yaşar
dc.contributor.authorSolmaz, Levent
dc.contributor.authorTanyıldızı, Şükrü Hanif
dc.date.accessioned2019-06-20T12:05:11Z
dc.date.available2019-06-20T12:05:11Z
dc.date.issued2018en_US
dc.identifier.issn0550-3213
dc.identifier.issn1873-1562
dc.identifier.urihttps://doi.org/10.1016/j.nuclphysb.2018.05.025
dc.identifier.urihttps://hdl.handle.net/20.500.12462/5503
dc.descriptionHiçyılmaz, Yaşar (Balikesir Author)en_US
dc.description.abstractWe consider the Higgs boson mass in a class of the UMSSM models in which the MSSM gauge group is extended by an additional U(1)' group. Implementing the universal boundary condition at the GUT scale we target phenomenologically interesting regions of UMSSM where the necessary radiative contributions to the lightest CP-even Higgs boson mass are significantly small and LSP is always the lightest neutralino. We find that the smallest amount of radiative contributions to the Higgs boson mass is about 50 GeV in UMSSM, this result is much lower than that obtained in the MSSM framework, which is around 90 GeV. Additionally, we examine the Higgs boson properties in these models in order to check whether if it can behave similar to the SM Higgs boson under the current experimental constraints. We find that enforcement of smaller radiative contribution mostly restricts the U(1)' breaking scale as v(S) less than or similar to 10 TeV. Besides, such low contributions demand h(S) similar to 0.2-0.45. Because of the model dependency in realizing these radiative contributions theta(E6) < 0 are more favored, if one seeks for the solutions consistent with the current dark matter constraints. As to the mass spectrum, we find that stop and stau can be degenerated with the LSP neutralino in the range from 300 GeV to 700 GeV; however, the dark matter constraints restrict this scale as m(<(t)over tilde>), m((tau) over tilde) greater than or similar to 500 GeV. Such degenerate solutions also predict stop-neutralino and stau-neutralino co-annihilation channels, which are effective to reduce the relic abundance of neutralino down to the ranges consistent with the current dark matter observations. Finally, we discuss the effects of heavy M-Z' in the fine-tuning. Even though the radiative contributions are significantly low, the required fine-tuning can still be large. We comment about reinterpretation of the fine-tuning measure in the UMSSM framework, which can yield efficiently low results for the fine-tuning the electroweak scaleen_US
dc.description.sponsorshipMarie Curie Action COFUND - 116C056 Balikesir University Scientific Research Projects - BAP-2017/142 BAP-2017/198en_US
dc.language.isoengen_US
dc.publisherElsevier Scienceen_US
dc.relation.isversionof10.1016/j.nuclphysb.2018.05.025en_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.rightsAttribution 3.0 United States*
dc.rights.urihttp://creativecommons.org/licenses/by/3.0/us/*
dc.subjectRenormalization-Group Equationsen_US
dc.subjectDark-Matteren_US
dc.subjectSupersymmetry-Breakingen_US
dc.subjectSymmetry-Breakingen_US
dc.subjectRelic Densityen_US
dc.subjectHiggsen_US
dc.subjectSusyen_US
dc.subjectMassen_US
dc.subjectParticleen_US
dc.subjectProgramen_US
dc.titleLeast fine-tuned U(1) extended SSMen_US
dc.typearticleen_US
dc.relation.journalNuclear Physics Ben_US
dc.contributor.departmentFen Edebiyat Fakültesien_US
dc.contributor.authorID0000-0002-0595-8803en_US
dc.contributor.authorID0000-0002-3222-7942en_US
dc.identifier.volume933en_US
dc.identifier.startpage275en_US
dc.identifier.endpage298en_US
dc.relation.tubitakinfo:eu-repo/grantAgreement/TUBITAK/2236en_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US


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