Quantifying the reheating temperature of the universe
Quantifying the reheating temperature of the universe
复制标题
量化宇宙的再加热温度
DOI：
10.1016/j.nuclphysb.2014.07.001
复制
发表时间：
2013
期刊：
影响因子：
--
通讯作者：
B. Zald'ivar
中科院分区：
文献类型：
--
作者：
A. Mazumdar;B. Zald'ivar
本文的目的是确定一个精确的定义的再热温度的一般微扰衰变的暴胀子。为了估计再热温度，需要满足两个重要条件：（a）暴胀子的衰变产物必须支配宇宙的能量密度，即宇宙成为完全辐射支配的，（B）暴胀子的衰变产物已经达到局部热力学平衡。对于某些参数的选择，后者是一个更严格的条件，这样的衰变产物可能会热化后的辐射开始支配。因此，我们得到的再热温度可以远低于标准的传说估计。在本文中，我们描述了在什么条件下，我们的宇宙可以有efficientorinefficientthermalisation，并量化的再热温度的情况。这一结果对许多依赖于宇宙热历史的应用产生了直接的影响，特别是引力子丰度。
The aim of this paper is to determine an exact definition of the reheat temperature for a generic perturbative decay of the inflaton. In order to estimate the reheat temperature, there are two important conditions one needs to satisfy: (a) the decay products of the inflaton must dominate the energy density of the universe, i.e. the universe becomes completely radiation dominated, and (b) the decay products of the inflaton have attained local thermodynamical equilibrium. For some choices of parameters, the latter is a more stringent condition, such that the decay products may thermalise much after the beginning of radiation–domination. Consequently, we have obtained that the reheat temperature can be much lower than the standard-lore estimation. In this paper we describe under what conditions our universe could haveefficientorinefficientthermalisation, and quantify the reheat temperature for both the scenarios. This result has an immediate impact on many applications which rely on the thermal history of the universe, in particular gravitino abundance.