Neutralino dark matter and other LHC predictions from quasi Yukawa unification

Shafi, Qaisar; Tanyıldızı, Şükrü Hanif; Ün, Cem Salih

doi:10.1016/j.nuclphysb.2015.09.019

“…The one-loop threshold corrections [2] [13] play an important role here. We estimate the unified Yukawa coupling at M GU T to be approximately 0.6 in MSSM (Figure 1), in agreement with previous work [14]. We then consider MSSM plus three (5 +5) multiplets and show a plot displaying gauge coupling unification ( Figure 2).…”

Section: Introductionsupporting

confidence: 86%

Masses of third family vectorlike quarks and leptons in Yukawa-unifiedE6

Hebbar

¹

,

Leontaris

²

,

Shafi

³

2016

Self Cite

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In supersymmetric E 6 the masses of the third family quarks and charged lepton, t − b − τ , as well as the masses of the vector-like quarks and leptons, D −D and L−L, may arise from the coupling 27 3 ×27 3 ×27 H , where 27 3 and 27 H denote the third family matter and Higgs multiplets respectively. We assume that the SO(10) singlet component in 27 H acquires a TeV scale VEV which spontaneously breaks U (1) ψ and provides masses to the vector-like particles in 27 3 , while the MSSM doublets in 27 H provide masses to t, b and τ . Imposing Yukawa coupling unification h t = h b = h τ = h D = h L at M GU T and employing the ATLAS and CMS constraints on the Z ψ boson mass, we estimate the lower bounds on the third family vector-like particles D −D and L −L masses to be around 5.85 TeV and 2.9 TeV respectively. These bounds apply in the supersymmetric limit.

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“…Historically, the case with µ > 0 was investigated far more in-depth, see [23][24][25][26][27][28][29][30][31][32][33][34][35][36]. The µ < 0 case was studied in e.g.…”

Section: Jhep06(2020)014mentioning

confidence: 99%

“…[49], this prompted a consideration of nonuniversal gaugino masses, see [37][38][39][41][42][43], with M 2 < 0. Such boundary conditions can most conveniently be achieved by considering Yukawa unification within the context of the Pati-Salam symmetry instead of fully unified SO (10), see [13,[35][36][37][38]50] for various Pati-Salam setups and studies of Yukawa unification. Another possible approach to g µ − 2 with µ < 0 is to only demand that the g µ − 2 prediction is no worse than in the Standard Model, see [40].…”

Section: Jhep06(2020)014mentioning

confidence: 99%

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Comparatively light extra Higgs states as signature of SUSY SO(10) GUTs with 3rd family Yukawa unification

Antusch

¹

,

Hohl

²

,

Susic

³

2020

J. High Energ. Phys.

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We study 3rd family Yukawa unification in the context of supersymmetric (SUSY) SO(10) GUTs and SO(10)-motivated boundary conditions for the SUSY-breaking soft terms. We consider µ < 0 such that the SUSY loop-threshold effects enable a good fit to all third family masses of the charged Standard Model (SM) fermions. We find that fitting the third family masses together with the mass of the SM-like Higgs particle, the scenario predicts the masses of the superpartner particles and of the extra Higgs states of the MSSM: while the sparticles are predicted to be comparatively heavy (above the present LHC bound but within reach of future colliders), the spectrum has the characteristic feature that the lightest new particles are the extra MSSM Higgses. We show that this effect is rather robust with respect to many deformations of the GUT boundary conditions, but turns out to be sensitive to the exactness of top-bottom Yukawa unification. Nevertheless, with moderate deviations of a few percent from exact top-bottom Yukawa unification (stemming e.g. from GUT-threshold corrections or higher-dimensional operators), the scenario still predicts extra MSSM Higgs particles with masses not much above 1.5 TeV, which could be tested e.g. by future LHC searches for ditau decays H 0 /A 0 → τ τ . Finding the extra MSSM Higges before the other new MSSM particles could thus be a smoking gun for a Yukawa unified SO(10) GUT.

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“…On the other hand, the dark matter is even more mysterious since very few information is known except the fact that it modifies galactic rotation, it is not baryonic, has no electric and color charges and do not interact with the light 36 , 37 . Apart from the particle candidates for the dark matter, such as supersymmetry neutralino, an interesting candidate has been provided by Chamseddine and Mukhanov.…”

Section: Introductionmentioning

confidence: 99%

Cosmology in the mimetic higher-curvature $$f(R,R_{\mu \nu }R^{\mu \nu })$$ gravity

Kaczmarek

¹

,

Szczęśniak

²

2021

Sci Rep

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In the framework of the mimetic approach, we study the $$f(R,R_{\mu \nu }R^{\mu \nu })$$ f ( R , R μ ν R μ ν ) gravity with the Lagrange multiplier constraint and the scalar potential. We introduce field equations for the discussed theory and overview their properties. By using the general reconstruction scheme we obtain the power law cosmology model for the $$f(R,R_{\mu \nu }R^{\mu \nu })=R+d(R_{\mu \nu }R^{\mu \nu })^p$$ f ( R , R μ ν R μ ν ) = R + d ( R μ ν R μ ν ) p case as well as the model that describes symmetric bounce. Moreover, we reconstruct model, unifying both matter dominated and accelerated phases, where ordinary matter is neglected. Using inverted reconstruction scheme we recover specific $$f(R,R_{\mu \nu }R^{\mu \nu })$$ f ( R , R μ ν R μ ν ) function which give rise to the de-Sitter evolution. Finally, by employing the perfect fluid approach, we demonstrate that this model can realize inflation consistent with the bounds coming from the BICEP2/Keck array and the Planck data. We also discuss the holographic dark energy density in terms of the presented $$f(R,R_{\mu \nu }R^{\mu \nu })$$ f ( R , R μ ν R μ ν ) theory. Thus, it is suggested that the introduced extension of the mimetic regime may describe any given cosmological model.

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Neutralino dark matter and other LHC predictions from quasi Yukawa unification

Cited by 15 publications

References 60 publications

Masses of third family vectorlike quarks and leptons in Yukawa-unifiedE6

Masses of third family vectorlike quarks and leptons in Yukawa-unifiedE6

Comparatively light extra Higgs states as signature of SUSY SO(10) GUTs with 3rd family Yukawa unification

Cosmology in the mimetic higher-curvature $$f(R,R_{\mu \nu }R^{\mu \nu })$$ gravity

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