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Inflaton mass in the nuMSM inflation
Anisimov, Alexey;Bartocci, Yannick;Bezrukov, Fedor L.
High Energy Physics - Phenomenology , 2008, DOI: 10.1016/j.physletb.2008.12.028
Abstract: We analyse the reheating in the modification of \nuMSM (Standard Model with three right handed neutrinos with masses below the electroweak scale) where the sterile neutrino providing the Dark Matter is generated in decays of the additional inflaton field. We deduce that due to rather inefficient transfer of energy from the inflaton to the Standard Model sector reheating tends to happen at very low temperature, thus providing strict bounds on the coupling between the inflaton and the Higgs particles. This in turn translates to the bound on the inflaton mass, which appears to be very light 0.1 GeV <~ m_I <~ 10 GeV, or slightly heavier then two Higgs masses 300 GeV <~ m_I <~ 1000 GeV.
Hybrid inflation with running inflaton mass  [PDF]
Laura Covi
Physics , 1998, DOI: 10.1103/PhysRevD.60.023513
Abstract: We realize and study a model of hybrid inflation in the context of softly broken supersymmetry. The inflaton is taken to be a flat direction in the superfield space and, due to unsuppressed couplings, its soft supersymmetry breaking mass runs with scale. Both gauge and Yukawa couplings are taken into account and different inflationary scenarios are investigated depending on the relative strenght of the couplings and the mass spectrum.
Ekpyrotic Reheating and Fate of Inflaton  [PDF]
HoSeong La
Physics , 2012,
Abstract: It is shown that perturbative reheating can reach a sufficiently high temperature with small or negligible inflaton decay rate provided that the inflaton potential becomes negative after inflation. In our model, inflaton and dark energy field are two independent scalar fields, and, depending on the mass of the inflaton and its coupling to matter fields, there is a possibility that the remaining inflaton after reheating can become a dark matter candidate.
Who is the Inflaton?  [PDF]
R. Brout
Physics , 2001,
Abstract: In the context of the two-fluid model introduced to tame the transplanckian problem of black hole physics, the inflaton field of the chaotic inflation scenario is identified with the fluctuation of the density of modes. Its mass comes about from the exchange of degrees of freedom between the two fluids.
Reheating Temperature and Inflaton Mass Bounds from Thermalization After Inflation  [PDF]
John McDonald
Physics , 1999, DOI: 10.1103/PhysRevD.61.083513
Abstract: We consider the conditions for the decay products of perturbative inflaton decay to thermalize. The importance of considering the full spectrum of inflaton decay products in the thermalization process is emphasized. It is shown that the delay between the end of inflaton decay and thermalization allows the thermal gravitino upper bound on the reheating temperature to be raised from 10^{8} GeV to as much as 10^{12} GeV in realistic inflation models. Requiring that thermalization occurs before nucleosynthesis imposes an upper bound on the inflaton mass as a function of the reheating temperature, m_{S} < 10^{10} (T_{R}/1 GeV)^{7/9} GeV. It is also shown that even in realistic inflation models with relatively large reheating temperatures, it is non-trivial to have thermalization before the electroweak phase transition temperature. Therefore the thermal history of the Universe is very sensitive to details of the inflation model.
Dark Matter from the Inflaton Field  [PDF]
A. de la Macorra
Physics , 2012, DOI: 10.1016/j.astropartphys.2011.11.009
Abstract: We present a model where inflation and Dark Matter takes place via a single scalar field phi. Without introducing any new parameters we are able unify inflation and Dark Matter using a scalar field phi that accounts for inflation at an early epoch while it gives a Dark Matter WIMP particle at low energies. After inflation our universe must be reheated and we must have a long period of radiation dominated before the epoch of Dark Matter. Typically the inflaton decays while it oscillates around the minimum of its potential. If the inflaton decay is not complete or sufficient then the remaining energy density of the inflaton after reheating must be fine tuned to give the correct amount of Dark Matter. An essential feature here, is that Dark Matter-Inflaton particle is produced at low energies without fine tuning or new parameters. This process uses the same coupling g as for the inflaton decay. Once the field phi becomes non-relativistic it will decouple as any WIMP particle, since n_phi is exponentially suppressed. The correct amount of Dark Matter determines the cross section and we have a constraint between the coupling $g$ and the mass $m_o$ of phi. The unification scheme we present here has four free parameters, two for the scalar potential V(phi) given by the inflation parameter lambda of the quartic term and the mass m_o. The other two parameters are the coupling $g$ between the inflaton phi and a scalar filed varphi and the coupling h between varphi with standard model particles psi or chi. These four parameters are already present in models of inflation and reheating process, without considering Dark Matter. Therefore, our unification scheme does not increase the number of parameters and it accomplishes the desired unification between the inflaton and Dark Matter for free.
Inflaton field governed universe from NKK theory of gravity: stochastic approach  [PDF]
Mariano Anabitarte,Jose Edgar Madriz Aguilar,Mauricio Bellini
Physics , 2005, DOI: 10.1140/epjc/s2005-02404-9
Abstract: We study a nonperturbative single field (inflaton) governed cosmological model from a 5D Noncompact Kaluza-Klein (NKK) theory of gravity. The inflaton field fluctuations are estimated for different epochs of the evolution of the universe. We conclude that the inflaton field has been sliding down its (quadratic) potential hill along all the evolution of the universe and a mass of the order of the Hubble parameter. In the model here developed the only free parameter is the Hubble parameter, which could be reconstructed in future from Super Nova Acceleration Probe (SNAP) data.
Of Inflation and the Inflaton  [PDF]
Robert Brout
Physics , 2010,
Abstract: Due to intra-field gravitational interactions, field configurations have a strong negative component to their energy density at the planckian and transplanckian scales, conceivably resulting in a sequestration of the transplanckian field degrees of freedom. Quantum fluctuations then allow these to tunnel into cisplanckian configurations to seed inflation and conventional observed physics: propagating modes of QFT in a geometry which responds to the existence of these new modes through the energy constraint of general relativity, H^2 = \rho/3. That this tunnelling results in geometries and field configurations that are homogeneous allows for an estimate of the mass of the inflaton, m=O(10^{-6}), and the amplitude of the inflaton condensate, \phiav=O(10), both consistent with phenomenology.
Multiple quantum collapse of the inflaton field and its implications on the birth of cosmic structure  [PDF]
Gabriel León,Adolfo De Unánue,Daniel Sudarsky
Physics , 2010, DOI: 10.1088/0264-9381/28/15/155010
Abstract: The standard inflationary account for the origin of cosmic structure is, without a doubt, extremely successful. However, it is not fully satisfactory as has been argued in [A. Perez, H. Sahlmann, and D. Sudarsky, Class. Quantum Grav., 23, 2317, (2006), arXiv:gr-qc/0508100]. The central point is that, in the standard accounts, the inhomogeneity and anisotropy of our universe seems to emerge, unexplained, from an exactly homogeneous and isotropic initial state through processes that do not break those symmetries. The proposal made there to address this shortcoming calls for a dynamical and self-induced quantum collapse of the original homogeneous and isotropic state of the inflaton. In this article, we consider the possibility of a multiplicity of collapses in each one of the modes of the Quantum Field. As we will see, the results are sensitive to a more detailed characterization of the collapse than those studied in the previous works, and in this regard two simple options will be studied. We find important constraints on the model, most remarkably on the number of possible collapses for each mode.
Condensation of Planckian Modes and the Inflaton  [PDF]
Robert Brout
Physics , 2003,
Abstract: To confront the transplanckian problem encountered in the backward extrapolation of the cosmological expansion of the momenta of the modes of quantum field theory, it is proposed that there is a reservoir, depository of transplanckian degrees of freedom. These are solicited by the cisplanckian modes so as to keep their density fixed and the total energy density of vacuum at a minimum. The mechanism is due to mode - reservoir interaction, whereupon virtual quantum processes give rise to an effective mode-mode attraction. A BCS condensate results. It has a massless and massy collective excitation, the latter identified with the inflaton. For an effective non dimensional mode-reservoir coupling constant, g approx 0.3, the order of magnitude of its mass is what is required to account for cosmological fluctuations i.e. O(10^-6 -> 10^-5)m_Planck.
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