Radiative corrections set up inflation: dynamical models

Barshay, Saul; Kreyerhoff, Georg

doi:10.1007/s002880050580

Cited by 6 publications

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“…The φ mass has been calculated, from the minimum of the potential, to be of the order of 10 11 GeV. [12,13]. The φ can constitute a significant part of dark matter throughout the present universe.…”

Section: 3)mentioning

confidence: 99%

Stronger neutrino interactions at extremely high energies and the muon anomalous magnetic moment

Barshay

Kreyerhoff

2002

Eur. Phys. J. C

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A specific model of parity-conserving lepton substructure is considered. We show that a positive-definite contribution to the muon (g − 2)/2 at the possible level of about 4 × 10 −9 , can be related to a significant increase in the interaction cross section for cosmic-ray neutrinos with energies above about 10 19 eV. The additional cross section at ∼ 10 20 eV is calculated to be ∼ 10 −29 cm 2 , which is about 100 times the standard weak-interaction cross section. The model involves an extremely massive, neutral lepton, with mL ∼ = 2 × 10 6 GeV fixed by the new contribution to (g − 2)/2.One may consider a recently measured small deviation[1] from the theoreticallycalculated value of the muon anomalous magnetic moment as an indication of possible new physics. [2] In doing so, it would be valuable if two conditions were fulfilled.(1) The sign of the experimental deviation is positive. The new physics should produce this sign unambiguously. That is, it should contribute to the anomalous magnetic moment a positive-definite quantity.(2) It would be useful if the new physics implied other definite physical processes which are directly calculable. Further, these processes should be accessible to exploration in current experiments. They may well be related to puzzling aspects of the present experimental situation in different areas.In this paper, we give and discuss the results of straight-forward calculations based upon hypothetical additional F 1 dynamics which relates the possible deviation in (g − 2)/2 for the muon to the possible occurrence of stronger-than-weak interactions for muon (and tau) neutrinos at very high energies, E ν > 10 19 eV. The latter possibility concerns the nature and origin of the particles which initiate the highestenergy cosmic-ray air showers, with energies up to about 10 20 eV. This issue will be under further intense study in on-going [3,4] and up-coming cosmic-ray experiments [5,6]. In the early classic review of QED [7], a variety of contributions to the muon (g − 2)/2 were calculated from hypothetical couplings to "exotic particles" (section F 1 That is, additional to the dynamics contained in QED and in the standard electroweak-QCD model.

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Section: 3)mentioning

confidence: 99%

Stronger neutrino interactions at extremely high energies and the muon anomalous magnetic moment

Barshay

Kreyerhoff

2002

Eur. Phys. J. C

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“…[3] this scale. Inflation approaches termination as φ "falls" to a calculated [3,1] potential minimum, F 2 taken here at about φ = φ c = 10 18 GeV. Consider, as an example of the mechanism, that bosonic quanta (S) with mass m S ∼ = 10…”

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confidence: 99%

“…It is noteworthy that a typical, initial [1,3] potential energy density is of this order of magnitude; in particular, λφ 4 →∼ 6×10 62 GeV 4 for φ →∼ M P and with a small self-coupling parameter λ ∼ 3 × 10 −14 [7,6]. An estimated order of magnitude of the time for conversion of the initial, inflaton potential ("vacuum") energy into S quanta is The above sequence for the appearance of radiation is meant to be illustrative of a possibility.…”

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confidence: 99%

“…Also, one can ask whether a spontaneous CP violation is related to the vacuum expectation value of a pseudoscalar field involved in the dynamics of inflation, and whether this dynamics might contain a reason for the actual, small value of the baryon to photon ratio, a few times 10 −10 (alternatively, for the empirical number of baryons, a few times 10 78 ). In this paper, we describe several properties of a model which contains a scalar inflaton field with a large vacuum expectation value [1, 2] at a calculated [3,1], potential minimum, and also a related pseudoscalar field, whose small vacuum expectation value breaks CP invariance spontaneously * barshay@kreyerhoff.de † …”

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confidence: 99%

“…F 2 The illustrative, renormalization-group calculations which explicitly give rise to an inflaton effective potential with a maximum and a minimum [3,1], involve radiative corrections to a λφ 4 potential in a model with self-coupled scalar (φ) and pseudoscalar (b) fields, and also a massive lepton (which decays into radiation) with a scalar coupling to φ and a pseudoscalar coupling to b.…”

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confidence: 99%

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Dark-Matter Particles and Baryons From Inflation and Spontaneous Cp Violation in the Early Universe

Barshay¹,

Kreyerhoff²

2006

Mod. Phys. Lett. A

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We present aspects of a model which attempts to unify the creation of cold dark matter, a CP-violating baryon asymmetry, and also a small, residual vacuum energy density, in the early universe. The model contains a primary scalar (inflaton) field and a primary pseudoscalar field, which are initially related by a cosmological, chiral symmetry. The nonzero vacuum expectation value of the pseudoscalar field spontaneously breaks CP invariance.There is a relevant open question in relation to a hypothetical, brief inflationary period in the expansion of the early universe, initiated by the energy density of a scalar field. The question is whether the energy density in cold dark matter, and a very small energy density in an effective cosmological constant can arise in the early universe from the fields involved in the dynamics of inflation. Also, one can ask whether a spontaneous CP violation is related to the vacuum expectation value of a pseudoscalar field involved in the dynamics of inflation, and whether this dynamics might contain a reason for the actual, small value of the baryon to photon ratio, a few times 10 −10 (alternatively, for the empirical number of baryons, a few times 10 78 ). In this paper, we describe several properties of a model which contains a scalar inflaton field with a large vacuum expectation value [1, 2] at a calculated [3,1], potential minimum, and also a related pseudoscalar field, whose small vacuum expectation value breaks CP invariance spontaneously * barshay@kreyerhoff.de †

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The inflaton as dark matter

Barshay

Kreyerhoff

1998

Eur. Phys. J. C

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Within the framework of an explicit dynamical model, in which we calculate the radiatively-corrected, tree-level potential that sets up inflation, we show that the inflaton can be a significant part of dark matter today. We exhibit potentials with both a maximum and a minimum. Using the calculated position of the potential minimum, and an estimate for fluctuations of the inflaton field in the early universe, we calculate a contribution to the matter energy density of (1−2)×10 −47 GeV 4 in the present universe, from cold inflatons with mass of about 6 × 10 9 GeV. We show that the inflaton might decay in a specific way, and we calculate a possible lifetime that is several orders of magnitude greater than the present age of the universe. Inflaton decay is related to an interaction which, together with a spontaneous breakdown of CP invariance at a cosmological energy scale, can give rise to a neutrino-antineutrino asymmetry just prior to the time of electroweak symmetry breaking.

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Radiative corrections set up inflation: dynamical models

Cited by 6 publications

References 0 publications

Stronger neutrino interactions at extremely high energies and the muon anomalous magnetic moment

Stronger neutrino interactions at extremely high energies and the muon anomalous magnetic moment

Dark-Matter Particles and Baryons From Inflation and Spontaneous Cp Violation in the Early Universe

The inflaton as dark matter

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