论文标题
通过原始磁场和CMB探测加热阶段
Probing the reheating phase through primordial magnetic field and CMB
论文作者
论文摘要
长期以来，人们一直认为通货膨胀的磁化是在我们宇宙中产生大规模磁场的最有希望的机制。但是，通常，此类模型在标准框架中困扰着反应或强耦合问题。本文表明，再加热阶段可以与CMB一起减轻这些问题起着至关重要的作用。假设在整个重新加热期间的电导率可以忽略不计，则经典的法拉第电磁诱导会大大改变磁场的动力学。我们的详细分析表明，这种物理现象不仅可以在没有任何理论问题的情况下观察到可行的大量磁化模型，而且还可以唯一地固定状态的扰动平均加速器方程，$ω__2=（p+2）/（p+2）/（p+2）$在重新加热的情况下，鉴于大型磁场的特定价值。该观察结果暗示，如果人们认为大规模磁场的当今强度为$ \ nathcal {p} _ {b0} _ {b0}^{b0}^{1} {1} {1 10^{-18} $G。我们的分析为通过再加热构成通货膨胀和磁化模型的新途径。
Inflationary magnetogenesis has long been assumed to be the most promising mechanism for producing large-scale magnetic fields in our universe. However, generically, such models are plagued with either backreaction or strong coupling problems within the standard framework. This paper has shown that the reheating phase can play a crucial role in alleviating those problems along with CMB. Assuming the electrical conductivity to be negligible during the entire period of reheating, the classic Faraday electromagnetic induction changes the magnetic field's dynamics drastically. Our detailed analysis reveals that this physical phenomenon not only converts a large class of magnetogenesis model observationally viable without any theoretical problem but also can uniquely fix the perturbative average inflaton equation of state, $ω_ϕ = (p+2)/(p+2)$ during reheating given a specific value of the large scale magnetic field. This observation hints the inflaton to assume the potential of form $V(ϕ) \sim ϕ^p$ near its minimum with $p \gtrsim 3.5$ if one considers the limit of the present-day strength of the large scale magnetic field to be $\mathcal{P}_{B0}^{\frac{1}{2}} \gtrsim 10^{-18}$ G. Our analysis opens up a new avenue towards constraining the inflationary and magnetogenesis model together via reheating.
