Warm inflation in the presence of magnetic fields

Abstract

We study the effects of primordial magnetic fields on the inflationary potential in the context of a warm inflation scenario. The model, based on global supersymmetry with a new-inflation-type potential and a coupling between the inflaton and a heavy intermediate superfield, is already known to preserve the flatness required for slow-roll conditions even after including thermal contributions. Here we show that the magnetic field makes the potential even flatter, retarding the transition and rendering it smoother.Comment: 13 pages, 10 figures. References added and discussion expanded. Version to be published in PR

Magnetic field effect on early universe events

“…For thermal corrections to the original model, see (Hall & Moss 2005), and for magnetic contributions, see (Piccinelli et al 2014; Piccinelli & Sánchez 2021). For both contributions, the flatness of the inflaton potential is not spoiled.…”

“…What events will then be affected? Among others: PTs ‐inflation (Piccinelli et al 2014), the EWPT, with its possibly associated baryogenesis process (Elmfors et al 1998; Giovannini & Shaposhnikov 1998; Kajantie et al 1999; Sanchez et al 2007), nucleosynthesis (BBN) (Grasso & Rubinstein 1996), the evolution of primordial perturbations (Barrow et al 2007; Kojima & Ichiki 2009).…”

Effect of a primordial magnetic field on the inflaton decay process in a warm inflation scenario

“…Once we compute the self-energies in Fig. 1, we obtain the leading order corrections, from thermal and magnetic effects, to the heavy sector boson and fermion masses which (for more details see Piccinelli et al (2014)) can be written as…”

“…Both quantities can be inferred from the heavy sector self-energy: the former needs the real part, while the last one is related to the imaginary part. The results for the effective potential have been already published (Piccinelli et al 2014) but we briefly expose them here for completeness; the dissipation coefficient part is work under progress and we present here the calculation for the decay width of the heavy boson to two light charged bosons, at finite temperature and in presence of a magnetic field.…”

A non-perturbative study of the evolution of cosmic magnetised sources

“…In the above mentioned articles on early times cosmological magneto-genesis the dynamics of the magnetic interaction in the cosmic fluid is examined by means of a variety of techniques and theoretical frameworks depending on the specific transition: numerical simulations, Kinetic Theory, Statistical Mechanics, or gauge invariant vector perturbations over a spatially flat FLRW background (see details in [8,9,10,11], see other approaches to primordial magnetism in [17,18,19]). However, a classical Maxwellian electromagnetic interaction (not necessarily restricted to early cosmic times) can also be incorporated into the full dynamics of General Relativity through an elegant first order system based on covariant objects defined in a 4-velocity frame (the 1+3 formalism [9,20,21]).…”