General inflaton potentials in supergravity

By R. Kallosh, Andrei Linde, Tomas Rube. 2010

269 citations recorded by the source corpus.

We describe a way to construct supergravity models with an arbitrary inflaton potential V({phi}) and show that all other scalar fields in this class of models can be stabilized at the inflationary trajectory by a proper choice of the Kaehler potential.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c9242b62069761542382f77f1da2146d6bc908fe

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Andrei Linde
2. R. Kallosh
3. J. J. Carrasco
4. D. Roest
5. E. Pajer
6. Sergio Ferrara
7. G. Dall’Agata
8. A. Westphal

In Nuclear and High Energy Physics

1. Andrei Linde
2. R. Kallosh
3. J. J. Carrasco
4. D. Roest
5. Sergio Ferrara
6. E. Pajer
7. G. Dall’Agata
8. A. Westphal

Citations in the corpus

• Observational consequences of chaotic inflation with nonminimal coupling to gravity (2011, background): “According to [4, 7], the evolution of this field is described by the theory of the scalar field φ nonminimally interacting with gravity, with ξ = −(1) 6 + χ 4 .”
• Inflationary Cosmology after Planck 2013 (2014, methodology): “After that, the proper choice of the Kähler potential can make it not only an extremum, but a minimum, thus stabilizing the inflationary regime [89, 90, 94].”
• α-attractors: Planck, LHC and dark energy (2015, background): “This was explained in [24, 25] developing on the pioneering work [26].”
• Universality class in conformal inflation (2013, methodology): “5) An advantage of this gauge is that we may use a well tested over the years Mathematica code [23], developed further in [24], and study moduli stabilization.”
• Inflation and uplifting with nilpotent superfields (2014, methodology): “Because of the additional term W0, this theory deviates from the structure of the models of [3] where we had W = Sf(Φ).”
• Cosmological attractors and initial conditions for inflation (2015, background): “if the goldstino superfield is nilpotent [13], or if it is strongly stabilized at S = 0 by terms ∼ (SS̄)(2) which can be added to the Kähler potential [24], [4].”
• Cosmology with nilpotent superfields (2014, methodology): “In all our supergravity models in [1–9], there is one light scalar, the inflaton.”
• Superconformal inflationary α-attractors (2013, background): “Since that time, we learned how to implement chaotic inflation with practically any desirable potential in supergravity with chiral matter multiplets [4] as well as in supergravity with vector and tensor multiplets [5].”
• On sgoldstino-less supergravity models of inflation (2014, methodology): “The first condition means that f(z) can be represented by a power series in (i z) with real coefficients, and is analogous to the requirement of a real holomorphic function made in [22, 24]: the difference just reflects the different convention on the embedding of φ in Φ with respect to (1.”
• Gauge field production in supergravity inflation: Local non-Gaussianity and primordial black holes (2012, methodology): “The new class of models [1–3] describes two scalar fields, S and Φ, with the superpotential”
• Hyperbolic geometry of cosmological attractors (2015, background): “This results in a broad class of chaotic inflation model in supergravity with nearly arbitrary inflaton potentials proposed in [8].”