雙光子散射與單光子衰變造成高磁化星體能量流失率之比較

Abstract

能量流失現象對於超新星的爆炸與中子星的產生是很重要的。在標準模型理論中，星體流失能量的主要機制是 plasmon 衰變 γ→νν。在另一方面，引進一個 scalar-scalar four-fermion interaction 在散射γγ→νν中，則會比它在標準模型理論中有更大的散射面積。 在本文中，我們會討論由於上面的γγ→νν作用，星體的能量流失率，然後將其與標準模型理論中的單光子衰變做比較。

Energy loss is an important phenomenon for the explosion of supernovae and the creation of neutron stars. The plasmon decay γ→νν is known to be the dominant stellar energy-loss mechanism in the standard model. On the other hand, the scattering γγ→νν, induced by the scalar-scalar four-fermion interaction has a much larger cross section than its counterpart in the standard model. In this document, we study the energy emission rate by the γγ→νν process in the model mentioned above, and compare this rate with that of the plasmon decay in the standard model.