TY - JOUR
T1 - Calculations of inflaton decays and reheating
T2 - With applications to no-scale inflation models
AU - Ellis, John
AU - Garcia, Marcos A.G.
AU - Nanopoulos, Dimitri V.
AU - Olive, Keith A.
N1 - Publisher Copyright:
© 2015 IOP Publishing Ltd and Sissa Medialab srl.
PY - 2015/7/1
Y1 - 2015/7/1
N2 - We discuss inflaton decays and reheating in no-scale Starobinsky-like models of inflation, calculating the effective equation-of-state parameter, w, during the epoch of inflaton decay, the reheating temperature, Treh, and the number of inflationary e-folds, N∗, comparing analytical approximations with numerical calculations. We then illustrate these results with applications to models based on no-scale supergravity and motivated by generic string compactifications, including scenarios where the inflaton is identified as an untwisted-sector matter field with direct Yukawa couplings to MSSM fields, and where the inflaton decays via gravitational-strength interactions. Finally, we use our results to discuss the constraints on these models imposed by present measurements of the scalar spectral index ns and the tensor-to-scalar perturbation ratio r, converting them into constraints on N∗, the inflaton decay rate and other parameters of specific no-scale inflationary models.
AB - We discuss inflaton decays and reheating in no-scale Starobinsky-like models of inflation, calculating the effective equation-of-state parameter, w, during the epoch of inflaton decay, the reheating temperature, Treh, and the number of inflationary e-folds, N∗, comparing analytical approximations with numerical calculations. We then illustrate these results with applications to models based on no-scale supergravity and motivated by generic string compactifications, including scenarios where the inflaton is identified as an untwisted-sector matter field with direct Yukawa couplings to MSSM fields, and where the inflaton decays via gravitational-strength interactions. Finally, we use our results to discuss the constraints on these models imposed by present measurements of the scalar spectral index ns and the tensor-to-scalar perturbation ratio r, converting them into constraints on N∗, the inflaton decay rate and other parameters of specific no-scale inflationary models.
KW - cosmological perturbation theory
KW - inflation
KW - particle physics - cosmology connection
KW - supersymmetry and cosmology
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U2 - 10.1088/1475-7516/2015/07/050
DO - 10.1088/1475-7516/2015/07/050
M3 - Article
AN - SCOPUS:84938311968
SN - 1475-7516
VL - 2015
JO - Journal of Cosmology and Astroparticle Physics
JF - Journal of Cosmology and Astroparticle Physics
IS - 7
M1 - 050
ER -