Understanding gravitational particle production in quintessential inflation

Abstract

The diagonalization method, introduced by a group of Russian scientists at the beginning of seventies, is used to compute the energy density of superheavy massive particles produced due to a sudden phase transition from inflation to kination in quintessential inflation models, the models unifying inflation with quintessence originally proposed by Peebles-Vilenkin. These superheavy particles must decay in lighter ones to form a relativistic plasma, whose energy density will eventually dominate the one of the inflaton field, in order to have a hot universe after inflation. In the present article we show that, in order that the overproduction of Gravitational Waves (GWs) during this phase transition does not disturb the Big Bang Nucleosynthesis (BBN) success, the decay has to be produced after the end of the kination regime, obtaining a maximum reheating temperature in the TeV regime.

arXiv comment18 pages, 5 figures. Version accepted for publication in JCAP

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Cited by in corpus (10)

• In the Realm of the Hubble tension $-$ a Review of Solutions
• Ability of LIGO and LISA to probe the equation of state of the early Universe
• A review of Quintessential Inflation
• Quintessential inflation in Palatini $f(R)$ gravity
• Quintessential Inflation from Lorentzian Slow Roll
• Gravitational production of superheavy baryonic and dark matter in quintessential inflation: nonconformally coupled case
• Cosmological consequences of a scalar field with oscillating equation of state. III. Unifying inflation with dark energy and small tensor-to-scalar ratio
• Constraining the quintessential $\alpha$-attractor inflation through dynamical horizon exit method
• Prediction of the Expansion of the Universe made by Alexander Friedmann and the Effect of Particle Creation in Cosmology
• Gravitational particle production of superheavy massive particles in Quintessential Inflation: A numerical analysis