Building models of inflation in no-scale supergravity

Ellis, John; García, Marcos A. G.; Nagata, Natsumi; Nanopoulos, Dimitri V.; Olive, Keith A.; Verner, Sarunas

doi:10.1142/s0218271820300116

Cited by 53 publications

(58 citation statements)

References 192 publications

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“…(18). In order to avoid these potential problems, we can follow the treatment presented in [31,44,52] and include an adjustable parameter for supersymmetry breaking and dark energy without invoking any additional fields. A full treatment of supersymmetry breaking and the electroweak transition lies beyond the scope of this paper and will be considered in future work.…”

Section: Non-oscillatory Effective Potentialmentioning

confidence: 99%

“…If we assume that the momentum values are negligibly small, the adiabaticity violation condition (31)…”

Section: The Equation Of Motion For the Higgs Field H In Fourier Spacmentioning

confidence: 99%

“…The theory of supergravity is characterized by the geometric properties of a non-trivial Kähler manifold, which can incorporate naturally the required effective interaction terms between the inflaton and the proxy Higgs field h. Further, we are motivated to study scenarios based on no-scale supergravity [24][25][26] because it avoids undesirable anti-de Sitter states and emerges in the effective low-energy limit of string compactification [28]. For some previous models combining the SM with no-scale models of inflation, see [29][30][31][32][33][34][35][36].…”

Section: Introductionmentioning

confidence: 99%

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Non-oscillatory no-scale inflation

Ellis

Nanopoulos

Olive

et al. 2021

J. Cosmol. Astropart. Phys.

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We propose a non-oscillatory no-scale supergravity model of inflation (NO-NO inflation) in which the inflaton does not oscillate at the end of the inflationary era. Instead, the Universe is then dominated by the inflaton kinetic energy density (kination). During the transition from inflation to kination, the Universe preheats instantly through a coupling to Higgs-like fields. These rapidly annihilate and scatter into ultra-relativistic matter particles, which subsequently dominate the energy density, and reheating occurs at a temperature far above that of Big Bang Nucleosynthesis. After the electroweak transition, the inflaton enters a tracking phase as in some models of quintessential inflation. The model predictions for cosmic microwave background observables are consistent with Planck 2018 data, and the density of gravitational waves is below the upper bound from Big Bang Nucleosynthesis. We also find that the density of supersymmetric cold dark matter produced by gravitino decay is consistent with Planck 2018 data over the expected range of supersymmetric particle masses.

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Section: Non-oscillatory Effective Potentialmentioning

confidence: 99%

“…If we assume that the momentum values are negligibly small, the adiabaticity violation condition (31)…”

Section: The Equation Of Motion For the Higgs Field H In Fourier Spacmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Non-oscillatory no-scale inflation

Ellis

Nanopoulos

Olive

et al. 2021

J. Cosmol. Astropart. Phys.

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“…It is also favored from a bottom-up standpoint, because the input soft supersymmetry-breaking scalar masses of squarks and sleptons vanish, providing natural mechanisms for suppressing flavor-changing interactions [29], as discussed below. Moreover, no-scale supergravity also has cosmological advantages, as it avoids the traps of anti-de Sitter vacua with negative vacuum energy (cosmological constant) and provides flat directions in field space that facilitate the construction of models of cosmological inflation [31].…”

Section: Introductionmentioning

confidence: 99%

“…Equations (30)(31)(32) provide three conditions on the masses M H C , M and M X , which can related to the GUT Higgs vev V through the couplings λ, λ , and g 5 respectively. As a result, if c 5 = 0 only one of the two GUT couplings λ or λ can be chosen as a free parameter.…”

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confidence: 99%

Low-energy probes of no-scale SU(5) super-GUTs

et al. 2021

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We explore the possible values of the $$\mu \rightarrow e \gamma $$ μ → e γ branching ratio, $$\text {BR}(\mu \rightarrow e\gamma )$$ BR ( μ → e γ ) , and the electron dipole moment (eEDM), $$d_e$$ d e , in no-scale SU(5) super-GUT models with the boundary conditions that soft supersymmetry-breaking matter scalar masses vanish at some high input scale, $$M_\mathrm{in}$$ M in , above the GUT scale, $$M_{\mathrm{GUT}}$$ M GUT . We take into account the constraints from the cosmological cold dark matter density, $$\Omega _{CDM} h^2$$ Ω CDM h 2 , the Higgs mass, $$M_h$$ M h , and the experimental lower limit on the lifetime for $$p \rightarrow K^+ \bar{\nu }$$ p → K + ν ¯ , the dominant proton decay mode in these super-GUT models. Reconciling this limit with $$\Omega _{CDM} h^2$$ Ω CDM h 2 and $$M_h$$ M h requires the Higgs field responsible for the charge-2/3 quark masses to be twisted, and possibly also that responsible for the charge-1/3 and charged-lepton masses, with model-dependent soft supersymmetry-breaking masses. We consider six possible models for the super-GUT initial conditions, and two possible choices for quark flavor mixing, contrasting their predictions for proton decay with versions of the models in which mixing effects are neglected. We find that $$\tau \left( p\rightarrow K^+ \bar{\nu }\right) $$ τ p → K + ν ¯ may be accessible to the upcoming Hyper-Kamiokande experiment, whereas all the models predict $$\text {BR}(\mu \rightarrow e\gamma )$$ BR ( μ → e γ ) and $$d_e$$ d e below the current and prospective future experimental sensitivities or both flavor choices, when the dark matter density, Higgs mass and current proton decay constraints are taken into account. However, there are limited regions with one of the flavor choices in two of the models where $$\mu \rightarrow e$$ μ → e conversion on a heavy nucleus may be observable in the future. Our results indicate that there is no supersymmetric flavor problem in the class of no-scale models we consider.

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Sequestered Inflation

Каллош

Linde

Wrase

et al. 2021

Fortschritte der Physik

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We construct supergravity models allowing to sequester the phenomenology of inflation from the Planckian energy scale physics. The procedure consists of two steps: At Step I we study supergravity models, which might be associated with string theory or M-theory, and have supersymmetric Minkowski vacua with flat directions. At Step II we uplift these flat directions to inflationary plateau potentials. We find certain conditions which ensure that the superheavy fields involved in the stabilization of the Minkowski vacua at Step I are completely decoupled from the inflationary phenomenology.

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Building models of inflation in no-scale supergravity

Cited by 53 publications

References 192 publications

Non-oscillatory no-scale inflation

Non-oscillatory no-scale inflation

Low-energy probes of no-scale SU(5) super-GUTs

Sequestered Inflation

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