Cosmological problems for spontaneously broken supergravity

Goncharov, A. S.; Linde, Andrei; Vysotsky, M. I.

doi:10.1016/0370-2693(84)90116-3

Cited by 157 publications

(147 citation statements)

References 21 publications

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“…Thus, their effective mass during inflation was not that small, and they could roll down to their minimum even if inflation was not very long [5,7]. However, as was argued by Goncharov, Linde and Vysotsky [8], this does not solve the problem since typically the minimum of the effective potential during inflation does not coincide with the minimum of the effective potential at the present time with an accuracy 10 −7 M p − 10 −10 M p . Recently this problem was investigated by Dine, Randall and Thomas [9], who have argued that the positions of the two minima may in fact coincide if one invokes some additional symmetries.…”

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confidence: 89%

Relaxing the cosmological moduli problem

1996

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Typically the moduli fields acquire mass m 2 φ = ±C 2 H 2 in the early universe, which shifts the position of the minimum of their effective potential and leads to an excessively large energy density of the oscillating moduli fields at the later stages of the evolution of the universe. This constitutes the cosmological moduli problem, or Polonyi field problem. We show that the cosmological moduli problem can be solved or at least significantly relaxed in the theories in which C ≫ 1, as well as in some models with C ≪ 1.

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confidence: 89%

Relaxing the cosmological moduli problem

1996

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“…For a recent discussion of a closely related issue see [19]. It is possible to overcome this problem by adding new light scalar fields, such as Polonyi fields, and then solving the cosmological moduli problem related to them, which bothered phenomenologists for more than 30 years [20][21][22][23][24]. One can do it, but it requires a special effort with stabilizing the new moduli and making them very massive, see e.g.…”

Section: Jhep03(2015)111mentioning

confidence: 99%

Inflation, de Sitter landscape and super-Higgs effect

Каллош

Linde

Scalisi

2015

J. High Energ. Phys.

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We continue developing cosmological models involving nilpotent chiral superfields, which provide a simple unified description of inflation and the current acceleration of the universe in the supergravity context. We describe here a general class of models with a positive cosmological constant at the minimum of the potential, such that supersymmetry is spontaneously broken in the direction of the nilpotent superfield S. In the unitary gauge, these models have a simple action where all highly non-linear fermionic terms of the classical Volkov-Akulov action disappear. We present masses for bosons and fermions in these theories. By a proper choice of parameters in this class of models, one can fit any possible set of the inflationary parameters n s and r, a broad range of values of the vacuum energy V 0 , which plays the role of the dark energy, and achieve a controllable level of supersymmetry breaking. This can be done without introducing light moduli, such as Polonyi fields, which often lead to cosmological problems in phenomenological supergravity.

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“…For the inflationary model building, it seems that supergravity theory is a natural framework [80,81]. However, supersymmetry-breaking scalar masses in a generic supergravity theory are of the same order as the gravitino mass, inducing the so-called η problem [17,82,83], where all the scalar masses are of the order of the Hubble parameter due to the large vacuum energy density during inflation [84]. There are two elegant solutions: no-scale supergravity [85][86][87][88][89][90][91] and shift symmetry in the Kähler potential [92][93][94][95][96][97][98][99][100][101].…”

Section: C2mentioning

confidence: 99%

Modified Lyth bound and implications of BICEP2 results

Gao

Gong

2015

Phys. Rev. D

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To reconcile the BICEP2 measurement on the tensor-to-scalar ratio r with Planck constraint, a large negative running of scalar spectral index n s is needed. So the inflationary observable such as n s should be expanded at least to the second-order slow-roll parameters for single-field inflationary models. The large value of r and the Lyth bound indicate that it is impossible to obtain the sub-Planckian excursion for the inflaton. However, we derive an absolutely minimal bound ∆φ/M Pl > r/2 on the inflaton excursion for single-field inflationary models, which can be applied to non-slow-roll inflationary models as well. This bound excludes the possibility of the small-field inflation with ∆φ < 0.1M Pl if the BICEP2 result on r stands and it opens the window of sub-Planckian excursion with ∆φ < M Pl even if r is as large as 0.1. To get the sub-Planckian excursion with ∆φ < 0.1M Pl , our modified bound requires r < 0.02. Using a fifth-order polynomial potential as an explicit example, we show that it not only agrees with the observational results, but also violates the Lyth bound.

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Cosmological problems for spontaneously broken supergravity

Cited by 157 publications

References 21 publications

Relaxing the cosmological moduli problem

Relaxing the cosmological moduli problem

Inflation, de Sitter landscape and super-Higgs effect

Modified Lyth bound and implications of BICEP2 results

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