Recombination Effects on Supernova Light Curves
Recombination Effects on Supernova Light Curves
复制标题
超新星光曲线的复合效应
DOI：
10.3847/1538-4357/ab218a
复制
发表时间：
2014
期刊：
影响因子：
--
通讯作者：
R. Sari
中科院分区：
文献类型：
--
作者：
T. Faran;Tomer Goldfriend;E. Nakar;R. Sari
II型超新星（SNe II）的光变曲线被认为受到发生在其包层中的氢复合的高度影响。在这项工作中，我们分析调查的过渡从一个完全电离的信封，部分重组的SN光变曲线和它的影响。其动机是建立基本的过程，在后期主导的演变时，重组发生在信封，但足够早，使56镍衰变是一个可以忽略不计的能源。我们考虑了光子通过包层的扩散，同时分析了电离分数和辐射与气体之间的耦合，发现复合的主要影响是对所观察到的温度的演变。在复合之前，温度下降相对较快，而在复合开始之后，它显著降低了观察到的温度随时间下降的速率。这种行为是观测到的光学波段变平的主要原因，对于一个典型的红超巨星爆炸，复合波在光球相的大部分时间里只会轻微地影响测热光度。此外，在一些SNe II中观察到的平台期不是重组的一般结果，它也取决于祖先的密度结构。这是对SNe II（P和L）中观察到的不同光变曲线衰变率的一种可能解释。
The light curves of Type II supernovae (SNe II) are believed to be highly affected by recombination of hydrogen that takes place in their envelopes. In this work, we analytically investigate the transition from a fully ionized envelope to a partially recombined one and its effects on the SN light curve. The motivation is to establish the underlying processes that dominate the evolution at late times when recombination takes place in the envelope, yet early enough so that 56Ni decay is a negligible source of energy. We consider the diffusion of photons through the envelope while analyzing the ionization fraction and the coupling between radiation and gas and find that the main effect of recombination is on the evolution of the observed temperature. Before recombination, the temperature decreases relatively fast, while after recombination starts it significantly reduces the rate at which the observed temperature drops with time. This behavior is the main cause for the observed flattening in the optical bands, where for a typical red supergiant explosion the recombination wave affects the bolometric luminosity only mildly during most of the photospheric phase. Moreover, the plateau phase observed in some SNe II is not a generic result of recombination, and it also depends on the density structure of the progenitor. This is one possible explanation for the different light-curve decay rates observed in SNe II (P and L).
影响因子：
4.8
作者：
J. Lyman;D. Bersier;P. James
通讯作者：
J. Lyman;D. Bersier;P. James