论文标题
核心倒塌超新星祖细胞周围的前爆炸前泡腾区
A pre-explosion extended effervescent zone around core collapse supernova progenitors
论文作者
论文摘要
我提出了一个场景，根据该方案，密集的紧凑型情节（CSM）是，许多核心倒塌超新星（CCSNE）的射出在爆炸爆炸后的几天之内与浓密区域爆炸后的几天内相撞，除了恒星风外，气体还无法达到逃逸速度。在红色超级巨星（RSG）恒星周围的泡腾区中，有从RSG表面附近弹出的致密团块，升至天文学单元的半径，然后倒退。我考虑了弹出团块的两个简单速度分布。我发现结合质量的密度可能是逃避风的数十倍，因此可以模仿很高的质量损失率。密集的泡沫紧凑型CSM区域可以（1）解释许多CCSNE的射出的碰撞与爆炸后几天密集的紧凑型CSM的碰撞，（2）如果恒星经历了强大的质量损失率，如果恒星经历了强大的探索前的前示例性活动，（3）（3）在可见的频带和（4）在可见的带中造成的尘埃造成的尘埃，并有效地构成了（4）良好的群体，并有效地构成了（4）sater的secter，并有效地构成了（4）的量化，并有效地构成了（4）的量化量。单位，如果存在。泡腾区可能存在数千年及以上，因此，泡腾的CSM模型消除了许多II型CCSN祖细胞的要求，以经历爆炸前几年至几个月的强劲爆发。
I propose a scenario according to which the dense compact circumstellar matter (CSM) that the ejecta of many core collapse supernovae (CCSNe) collide with within several days after explosion results from a dense zone where in addition to the stellar wind there is gas that does not reach the escape velocity. In this effervescent zone around red supergiant (RSG) stars, there are dense clumps that are ejected from the vicinity of the RSG surface, rise to radii of tens of astronomical units, and then fall back. I consider two simple velocity distributions of the ejected clumps. I find that the density of the bound mass can be tens of times that of the escaping wind, and therefore can mimic a very high mass loss rate. The dense effervescent compact CSM zone can (1) explain the collision of the ejecta of many CCSNe with a dense compact CSM days after explosion, (2) facilitate very high mass loss rate if the star experiences powerful pre-explosion activity, (3) form dust that obscures the progenitor in the visible band, and (4) lead to an efficient mass transfer to a stellar companion at separations of tens of astronomical units, if exists. The effervescent zone might exist for thousands of years and more, and therefore the effervescent CSM model removes the requirement from many type II CCSN progenitors to experience a very strong outburst just years to months before explosion.
