![]() ![]() We have taken H I = m ϕ and λ I = 10 − 3. Different line styles correspond to different values of the unblocked decay rate Γ 0 = 0.1 m ϕ (solid, left panel), Γ 0 = 0.01 m ϕ (dashed, left panel), Γ 0 = 10 − 3 m ϕ (dash dot, right panel) and Γ 0 = 10 − 4 m ϕ (dotted, right panel). Results are shown as a function of the number of e-folds N after inflation for three different values of the Yukawa coupling, y = 0.01 (blue), 0.1 (red), and 1 (green). ![]() 4, calculated assuming slow oscillations ( τ Higgs ≫ H − 1). 11Tsung-Dao Lee Institute (TDLI), Shanghai Jiao Tong University, 200240 Shanghai, Chinaįor the case of perturbative inflaton decay: the ratio of the Bardeen parameter ζ rapid ( N ) calculated under the assumption of rapid Higgs oscillations ( τ Higgs ≪ H − 1) to the Bardeen parameter ζ in the right panel of Fig.10INFN, Laboratori Nazionali di Frascati, C.P.9Institute for Fundamental Physics of the Universe (IFPU), via Beirut 2, 34151 Trieste, Italy.8INFN, Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy.7Scuola Internazionale Superiore di Studi Avanzati (SISSA), via Bonomea 265, 34136 Trieste, Italy.6Institute Lorentz of Theoretical Physics, University of Leiden, 2333CA Leiden, Netherlands.5Nikhef, Science Park 105, 1098 XG Amsterdam, Netherlands.4Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), Campus UAB, 08193 Bellaterra, Barcelona.3Nordita, KTH Royal Institute of Technology and Stockholm University Roslagstullsbacken 23, 10691 Stockholm, Sweden.2Department of Physics, University of Texas, Austin, Texas 78722, USA.1The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, 10691 Stockholm, Sweden. ![]() For the case of resonant particle production (preheating) to (Higgsed) SM gauge bosons, we find temperature fluctuations larger than observed in the cosmic microwave background for a range of gauge coupling that includes those found in the SM and conclude that such preheating cannot be the main source of reheating the Universe after inflation.Īliki Litsa 1,*, Katherine Freese 1,2,3,†, Evangelos I. The strongest bounds arise in the case of reheating to top quarks where we find T reh ≲ O ( 10 12 ) GeV for an inflaton mass of 10 13 GeV. For the case of perturbative decay from coherent oscillations of the inflaton after high scale inflation, we find strong upper bounds on the reheat temperature for the inflaton decay into heavy SM particles. We consider both perturbative and resonant decay of the inflaton to SM particles. #BOSON X UNBLOCKED PATCH#As a light spectator field, the SM Higgs boson acquires large field values from its quantum fluctuations during inflation, gives masses to SM particles that vary from one Hubble patch to another, and thereby produces large density fluctuations. Cosmic microwave background observations are used to constrain reheating to standard model (SM) particles after a period of inflation. ![]()
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