Influence of interactions on particle production induced by time-varying mass terms

Enomoto, Seishi; Fuksinska, Olga; Lalak, Zygmunt

doi:10.1007/jhep03(2015)113

Cited by 7 publications

(12 citation statements)

References 13 publications

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“…Obviously, this depends on α and the properties of the ψ particles. A similar effect is achieved by inelastic scatterings, which have not been considered in [70] and related studies [71,72]. This implies that the nonperturbative particle production depends on the particle physics model into which V(ϕ) and L int are embedded.…”

Section: Parametric Resonance and Combined Reheatingmentioning

confidence: 69%

What can the CMB tell about the microphysics of cosmic reheating?

Drewes

2016

J. Cosmol. Astropart. Phys.

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In inflationary cosmology, cosmic reheating after inflation sets the initial conditions for the hot big bang. We investigate how CMB data can be used to study the effective potential and couplings of the inflaton during reheating and constrain the underlying microphysics. If there is a phase of preheating that is driven by a parametric resonance or other instability, then the thermal history and expansion history during the reheating era depend on a large number of microphysical parameters in a complicated way. In this case the connection between CMB observables and microphysical parameters can only established with intense numerical studies. Such studies can help to improve CMB constraints on the effective inflaton potential in specific models, but parameter degeneracies usually make it impossible to extract meaningful best-fit values for individual microphysical parameters. If, on the other hand, reheating is driven by perturbative processes, then it can be possible to constrain the inflaton couplings and the reheating temperature from CMB data. This provides an indirect probe of fundamental microphysical parameters that most likely can never be measured directly in the laboratory, but have an immense impact on the evolution of the cosmos by setting the stage for the hot big bang.

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Section: Parametric Resonance and Combined Reheatingmentioning

confidence: 69%

What can the CMB tell about the microphysics of cosmic reheating?

Drewes

2016

J. Cosmol. Astropart. Phys.

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“…where s denotes the fermionic helicity and ± distinguish between the particle and antiparticle. For more precise and detailed formulae see [7]. There is some physical meaning behind the formulae for the distributions in massless case -one can link the diagrams of the inverse decay processes ( Obtained numerical results for the number density of produced species are presented in Figures 5 and 6.…”

Section: Resultsmentioning

confidence: 99%

“…So far produced states just propagate and backreact on the background field but they do not interact. The role of the interactions and their effect on the amount of produced states is of great interest as it may change the final number density abundantly [7].…”

Section: The Role Of Interactionsmentioning

confidence: 99%

Particle production in the background with VEV depending on time

Czerwińska¹,

Enomoto²,

Lalak³

2016

Proceedings of 18th International Conference From the Planck Scale to the Electroweak Scale — PoS(PLANCK 2015)

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“…e.g. [57][58][59] for specific examples. Feedback typically becomes relevant when the occupation numbers in the plasma reach unity.…”

Section: Reheating As a Key To Fundamental Physicsmentioning

confidence: 99%

Measuring the Inflaton Coupling in the CMB

Drewes

2019

Preprint

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We study under which conditions it is possible to establish analytic relations between CMB observables and the inflaton coupling to radiation. The crucial criterion is that the dissipation at the end of the reheating phase must be primarily driven by perturbative decays. When reheating is primarily driven by interactions that are linear in the inflaton field, then this is possible if the coupling constant is, roughly speaking, smaller than the ratio between the inflaton mass and the Planck mass. For interactions involving higher powers of the inflaton field the range of observationally accessible parameter values is generally smaller. The size of the inflaton coupling is not only interesting for particle physics model building, but crucially shapes the evolution of the cosmos by setting the initial condition for the hot big bang when reheating the universe.

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Influence of interactions on particle production induced by time-varying mass terms

Cited by 7 publications

References 13 publications

What can the CMB tell about the microphysics of cosmic reheating?

What can the CMB tell about the microphysics of cosmic reheating?

Particle production in the background with VEV depending on time

Measuring the Inflaton Coupling in the CMB

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