Reheating Temperature after Inflation in No-Scale Supergravity

TL;DR

This paper investigates the reheating temperature after inflation within a No-Scale Supergravity framework, analyzing decay processes and mechanisms that lead to a reheating temperature around 10^{10} GeV, crucial for early universe cosmology.

Contribution

It introduces a detailed analysis of preheating mechanisms in No-Scale Supergravity, combining inflaton decay and scattering processes to estimate reheating temperatures.

Findings

Reheating temperature estimated at ~10^{10} GeV.

Both decay and scattering mechanisms are essential for preheating.

Inflaton decay and scattering processes contribute comparably to reheating.

Abstract

By using a No-Scale Supergravity model, which was proved well to explain WMAP observations appropriately, a mechanism of preheating just after the end of inflation is investigated. By using the canonically normalized and diagonalized scalars, the decay rates of these fields are calculated inflaton $S$ into gauge sector fields. The reheating temperature is estimated by both the stability condition of Boltzmann equation and the instant preheating mechanism. The both of reheating temperatures are almost the same order of magnitude $\sim O(10^{10})$ GeV. Because two mechanisms are completely independent processes, the former is caused through the inflaton decays into gauge fields and gauginons and the latter is caused by the scattering process of two inflatons into two right handed sneutrinos, which will decay into Higgs fields and other minimal SUSY standard model (MSSM) particles, we conclude that both mechanisms play essential roles in the preheating process after inflation.