标题： 热膨胀与模问题 显示英文标题

标题： Thermal Inflation and the Moduli Problem

摘要： 在超对称理论中，一个场可以发展出真空期望值$M \gg 10^3\,{\rm GeV}$，尽管其质量$m$与$10^2$相当，到$10^3\,{\rm GeV}$。 早期宇宙中的有限温度可以使该场保持为零，对应于能量密度为$ V_0 \sim m^2 M^2 $的假真空。 当温度降至$V_0^{1/4}$以下时，热能密度变得可以忽略，并开始一个热暴胀时期。 它在温度约为$m$时结束，对应约 10$e$倍的暴胀，这不会影响普通暴胀期间产生的密度扰动。 如果$M$在$10^{12}\,{\rm GeV}$的一到两个数量级范围内，热暴胀可以解决Polonyi/模问题。 显示英文摘要

摘要： In supersymmetric theories a field can develop a vacuum expectation value $M \gg 10^3\,{\rm GeV}$, even though its mass $m$ is of order $10^2$ to $10^3\,{\rm GeV}$. The finite temperature in the early Universe can hold such a field at zero, corresponding to a false vacuum with energy density $ V_0 \sim m^2 M^2 $. When the temperature falls below $V_0^{1/4}$, the thermal energy density becomes negligible and an era of thermal inflation begins. It ends when the field rolls away from zero at a temperature of order $m$, corresponding to of order 10 $e$-folds of inflation which does not affect the density perturbation generated during ordinary inflation. Thermal inflation can solve the Polonyi/moduli problem if $M$ is within one or two orders of magnitude of $10^{12}\,{\rm GeV}$.