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Wess-Zumino Inflation in Light of Planck
Cosmology and Nongalactic Astrophysics · Submitted 25 Mar 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim With suitable parameters and assuming a plausible initial condition at the start of the inflationary epoch, the model can yield scalar perturbations in the Cosmic Microwave Background (CMB) of the correct strength with a spectral index n_s ~ 0.96 and a tensor-to-scalar perturbation ratio r < 0.1, consistent with the Planck CMB data.
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The abstract, sentence by sentence
We discuss cosmological inflation in the minimal Wess-Zumino model with a single massive chiral supermultiplet. With suitable parameters and assuming a plausible initial condition at the start of the inflationary epoch, the model can yield scalar perturbations in the Cosmic Microwave Background (CMB) of the correct strength with a spectral index n_s ~ 0.96 and a tensor-to-scalar perturbation ratio r < 0.1, consistent with the Planck CMB data. We also discuss the possibility of topological inflation within the Wess-Zumino model, and the possibility of combining it with a seesaw model for neutrino masses. This would violate R-parity, but at such a low rate that the lightest supersymmetric particle would have a lifetime long enough to constitute the astrophysical cold dark matter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We discuss cosmological inflation in the minimal Wess-Zumino model with a single massive chiral supermultiplet. | contribution 0.80 | 0.70 | 0.05 | asserted 0.60 |
| s1 | With suitable parameters and assuming a plausible initial condition at the start of the inflationary epoch, the model can yield scalar perturbations in the Cosmic Microwave Background (CMB) of the correct strength with a spectral index n_s ~ 0.96 and a tensor-to-scalar perturbation ratio r < 0.1, consistent with the Planck CMB data. | result 0.99 | 0.70 | 0.81 | hedged possibility 1.00 |
| s2 | We also discuss the possibility of topological inflation within the Wess-Zumino model, and the possibility of combining it with a seesaw model for neutrino masses. | contribution 0.94 | 0.59 | 0.05 | hedged possibility 0.96 |
| s3 | This would violate R-parity, but at such a low rate that the lightest supersymmetric particle would have a lifetime long enough to constitute the astrophysical cold dark matter. | interpretation 0.62 | 0.26 | 0.09 | asserted 0.76 |
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The paper
Original abstract
We discuss cosmological inflation in the minimal Wess-Zumino model with a single massive chiral supermultiplet. With suitable parameters and assuming a plausible initial condition at the start of the inflationary epoch, the model can yield scalar perturbations in the Cosmic Microwave Background (CMB) of the correct strength with a spectral index n_s ~ 0.96 and a tensor-to-scalar perturbation ratio r < 0.1, consistent with the Planck CMB data. We also discuss the possibility of topological inflation within the Wess-Zumino model, and the possibility of combining it with a seesaw model for neutrino masses. This would violate R-parity, but at such a low rate that the lightest supersymmetric particle would have a lifetime long enough to constitute the astrophysical cold dark matter.
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References
How the literature uses it
42 arXiv papers cite this in 69 sentences
Papers citing it · 46 sentences without a confident label
Contests it 1 paper
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On parameterizing the field as $ϕ→x v$, where $x$ is dimensionless, for the chosen potential in [ref] , the inflationary observables reduce to[In [ref] , a minus sign is missing in the expression for $N$.
Reanalyzing the upper limit on the tensor-to-scalar perturbation ratio r_T in a quartic potential inflationary model · Inflaton Potential and Background Dynamics · contest 0.90
Builds on it 3 papers
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Accordingly, we first explore how the results of [ref] can be generalized if one chooses $v = 40$ but allows initial conditions with $σ0$.
Exploring Two-Field Inflation in the Wess-Zumino Model · Predictions for $n_s$ and $r$ · 0.97
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In this paper we show how one can elevate the simplest globally-supersymmetric Wess-Zumino inflationary model of [ref] to a no-scale supergravity version (NSWZ).
No-Scale Supergravity Realization of the Starobinsky Model of Inflation · Introduction · 0.99
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In this case, an interesting application of the analysis in this paper is in SUSY models which realize leptogenesis through an $N^3$ term in the superpotential [ref] .
Stability, reheating and leptogenesis · Discussion · 0.81
Uses its data or values 1 paper
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(the solution found in [ref] ), at $ψ∼-15.5$, $ψ̂∼- 0.39$, and at an equivalent pair of points that are their mirror images under reflection in the symmetry axis.
Exploring Two-Field Inflation in the Wess-Zumino Model · Predictions for $n_s$ and $r$ · 0.84
Compares with it 3 papers
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The results for $v=40$ and $v=26$ can be compared with Table 1 of [ref]
Exploring Two-Field Inflation in the Wess-Zumino Model · Predictions for $n_s$ and $r$ · 0.97
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The results in Ref. [ref] are similar to our model with $ϕ^2e^-βϕ$ shown in Fig. [ref].
Supergravity Inflation with Broken Shift Symmetry and Large Tensor-to-Scalar Ratio · Numerical Results · 1.00
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In [ref] , a similar scalar potential was obtained using a minimal Wess-Zumino model with a single superfield.
Realize cosmological inflation in supersymmetric Grand Unified models with $R$-symmetry breaking · General discussions · 0.94
Cites it as support 1 paper
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Remarkably, the simplest single-field, globally-supersymmetric Wess-Zumino model has an effective potential that can inflate successfully in agreement with Planck data [ref] , as seen in Fig. [ref].
Summary of the Nobel Symposium on LHC Results · Cosmological Inflation in Light of Planck · 0.97
Cites it as background 11 papers
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Recently, it was shown that, within a Wess-Zumino framework, where the superpotential consists of quadratic and cubic terms only [ref] , no-scale SUGRA can behave like a Starobinsky inflationary model [ref] (see also [ref] for a realisation within an $SO(10)$ model, and for other No-Scale inflation realisations [ref] ).
Starobinsky-like inflation in no-scale supergravity Wess-Zumino model with Polonyi term · Introduction and Motivation · 0.80
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The chaotic inflation model in supergravity was proposed in Ref. [ref] , where an approximate shift symmetry on the inflaton was introduced to have good control over inflaton field values greater than the Planck scale.[ There are various large-field inflation models in the supergravity and superstring theory [ref] . ]
Gravitino Problem in Supergravity Chaotic Inflation and SUSY Breaking Scale after BICEP2 · Introduction · 0.80
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The simplest globally-supersymmetric model is the Wess-Zumino model with a single chiral superfield $Φ$ [ref] , which is characterized by a mass term $μ̂$ and a trilinear coupling $λ$, with the superpotential [equation] As was discussed in [ref] , the effective potential of the Wess-Zumino model reduces to ([ref]) when the imaginary part of the scalar component of $Φ$ vanishes, in which case this model yields Planck-compatible inflation for a suitable small value of $λ$.
No-Scale Supergravity Realization of the Starobinsky Model of Inflation · Introduction · 0.90
What it cites · 23 sentences without a confident label
Uses data or values from 1 paper
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This disfavouring of $ϕ^n$ models with $n≥2$ has been reinforced by the Planck data, which provide the strengthened upper limit $r < 0.11$ and constrain $n_s = 0.9603 ±0.0073$ [ref] .
Planck 2013 results. XXII. Constraints on inflation · Introduction and Summary · 0.96
Cites as background 4 papers
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Models with potentials of the form $αϕ^2 + βϕ^4$ with positive coefficients interpolate between pure $ϕ^2$ and $ϕ^4$ models and are therefore also disfavoured [There has been interest in models with a linear potential $∝ϕ$ [ref] , and even in models with a fractional power of $ϕ$ [ref] , though these can only be considered as effective models [ref] .].
Monodromy in the CMB: Gravity Waves and String Inflation · Introduction and Summary · 0.93
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Models with potentials of the form $αϕ^2 + βϕ^4$ with positive coefficients interpolate between pure $ϕ^2$ and $ϕ^4$ models and are therefore also disfavoured [There has been interest in models with a linear potential $∝ϕ$ [ref] , and even in models with a fractional power of $ϕ$ [ref] , though these can only be considered as effective models [ref] .].
Gravity Waves and Linear Inflation from Axion Monodromy · Introduction and Summary · 0.93
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Models with potentials of the form $αϕ^2 + βϕ^4$ with positive coefficients interpolate between pure $ϕ^2$ and $ϕ^4$ models and are therefore also disfavoured [There has been interest in models with a linear potential $∝ϕ$ [ref] , and even in models with a fractional power of $ϕ$ [ref] , though these can only be considered as effective models [ref] .].
Constraining Monodromy Inflation · Introduction and Summary · 0.93
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