Abstract

Superbursts of neutron stars are rare but powerful events explained by the explosive burning of carbon in the deep layers of the outer envelope of the star. In this paper we perform a simulation of superbursts and propose a simple method for describing the neutrino stage of their cooling, as well as a method for describing the evolution of the burst energy on a scale of several months. We note a universal relation for the temperature distribution in the burnt layer at its neutrino cooling stage, as well as the unification of bolometric light curves and neutrino heat loss rates for deep and powerful bursts. We point out the possibility of long-term retention of the burst energy in the star’s envelope. The results can be useful for interpretation of superburst observations.

中文翻译：

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中子星超爆发的中微子发射

摘要

中子星超级爆发是罕见但强大的事件，可以用恒星外壳深层碳的爆炸性燃烧来解释。在本文中，我们对超级爆发进行了模拟，并提出了一种描述中微子冷却阶段的简单方法，以及描述几个月规模的爆发能量演化的方法。我们注意到中微子冷却阶段燃烧层温度分布的普遍关系，以及深度和强大爆发的辐射热光曲线和中微子热损失率的统一。我们指出爆发能量长期保留在恒星包层中的可能性。结果可用于解释超暴观测。