Beginning of Universe through large field hybrid inflation

Kobayashi, Tatsuo; Seto, Osamu

doi:10.1142/s0217732315501060

Cited by 6 publications

(6 citation statements)

References 58 publications

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“…The question how large r = O(0.1) may be obtained in specific models of hybrid inflation has been discussed in previous studies (see e.g. [13][14][15][16][17]).…”

Section: Introductionmentioning

confidence: 96%

False vacuum energy dominated inflation with largerand the importance of κ_s

Antusch¹,

Cefalà²,

Nolde³

et al. 2014

J. Cosmol. Astropart. Phys.

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We investigate to which extent and under which circumstances false vacuum energy (V 0 ) dominated slow-roll inflation is compatible with a large tensor-to-scalar ratio r = O(0.1), as indicated by the recent BICEP2 measurement. With V 0 we refer to a constant contribution to the inflaton potential, present before a phase transition takes place and absent in the true vacuum of the theory, like e.g. in hybrid inflation. Based on model-independent considerations, we derive an upper bound on the possible amount of V 0 domination and highlight the importance of higher-order runnings of the scalar spectral index (beyond α s ) in order to realise scenarios of V 0 dominated inflation. We study the conditions for V 0 domination explicitly with an inflaton potential reconstruction around the inflaton field value 50 e-folds before the end of inflation, taking into account the present observational data. To this end, we provide the up-to-date parameter constraints within ΛCDM + r + α s + κ s using the cosmological parameter estimation code Monte Python together with the Boltzmann code CLASS. 1

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“…The question how large r = O(0.1) may be obtained in specific models of hybrid inflation has been discussed in previous studies (see e.g. [13][14][15][16][17]).…”

Section: Introductionmentioning

confidence: 96%

False vacuum energy dominated inflation with largerand the importance of κ_s

Antusch¹,

Cefalà²,

Nolde³

et al. 2014

J. Cosmol. Astropart. Phys.

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“…In Ref. [22], a double inflation scenario has been proposed which is compatible with the BICEP2 data [17]. The first stage of inflation is of the SUSY hybrid type, while the second stage is left unspecified, which makes the scenario incomplete.…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from double hybrid inflation

Lazarides¹,

Panagiotakopoulos

2015

Phys. Rev. D

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We present a two stage hybrid inflationary scenario in non-minimal supergravity which can predict values of the tensor-to-scalar ratio of the order of few × 10 −2 . For the parameters considered, the underlying supersymmetric particle physics model possesses two inflationary paths, the trivial and the semi-shifted one. The trivial path is stabilized by supergravity corrections and supports a first stage of inflation with a limited number of e-foldings. The tensor-to-scalar ratio can become appreciable while the value of the scalar spectral index remains acceptable as a result of the competition between the relatively mild supergravity corrections and the strong radiative corrections to the inflationary potential. The additional number of e-foldings required for solving the puzzles of hot big bang cosmology are generated by a second stage of inflation taking place along the semi-shifted path. This is possible only because the semi-shifted path is almost perpendicular to the trivial one and, thus, not affected by the strong radiative corrections along the trivial path and also because the supergravity effects remain mild. The requirement that the running of the scalar spectral index remains acceptable limits the possible values of the tensor-to-scalar ratio not to exceed about 5 × 10 −2 . Our model predicts the formation of an unstable string-monopole network, which may lead to detectable gravity wave signatures in future space-based laser interferometer observations.

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“…To construct the exact cosmological solutions of equations ( 6)-( 9) for the case V = 0 we consider the scalar fields satisfying equation (7) as…”

Section: New Methods Of Exact Solutions Construction For Non-constant...mentioning

confidence: 99%

“…As for the model under consideration Sec. 4, the kinetic energies of scalar fields φ and χ are not restricted by the slow-roll regime, since their substitution from ( 25)-( 26) into (7) imply the satisfaction of any condition on Ḣ including Ḣ ≃ 0.…”

Section: The Effective Cosmological Constantmentioning

confidence: 99%

New method of exponential potentials reconstruction based on given scale factor in phantonical two-field models

Fomin,

Chervon

2021

Preprint

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We study cosmological dynamic equations of two-field phantonical models, using standard approach for constant potential in finding exact solutions. New method we proposed for reconstruction non-constant exponential potentials supporting given evolution of scale factor. The exact solutions for different types of inflation represented in explicit form. Criteria for limiting possible types of inflationary dynamics are formulated within the framework of the proposed approach. It is shown that these models explain both stages of the accelerated expansion of the universe.

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Beginning of Universe through large field hybrid inflation

Cited by 6 publications

References 58 publications

False vacuum energy dominated inflation with largerand the importance of κ_s

False vacuum energy dominated inflation with largerand the importance of κ_s

Gravitational waves from double hybrid inflation

New method of exponential potentials reconstruction based on given scale factor in phantonical two-field models

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Beginning of Universe through large field hybrid inflation

Cited by 6 publications

References 58 publications

False vacuum energy dominated inflation with largerand the importance of κs

False vacuum energy dominated inflation with largerand the importance of κs

Gravitational waves from double hybrid inflation

New method of exponential potentials reconstruction based on given scale factor in phantonical two-field models

Contact Info

Product

Resources

About

False vacuum energy dominated inflation with largerand the importance of κ_s

False vacuum energy dominated inflation with largerand the importance of κ_s