论文标题
IIN型超新星祖细胞的第一和第二质量爆发之间的比较
Comparison between the first and second mass eruptions from progenitors of Type IIn supernovae
论文作者
论文摘要
一些巨大的恒星经历了发作和强烈的质量损失阶段，其发光度波动。弹射材料形式的恒星周围的构图，随后的核心崩溃导致IIN类型超新星的特征是超新星喷射和情节物质之间的相互作用。尚未清楚地解释触发这些质量喷发和流出动态的能源。此外，如果重复这些事件，质量喷发本身可以改变包膜的密度结构，并影响随后的质量喷发的动力学。大量的观察证据表明，在核心崩溃之前进行了多次质量爆发。与第一个事件相比，我们研究了第一次质量喷发改变的包膜的密度结构以及随后的第二次质量喷发事件的性质。我们将额外的能量沉积在15 $ m_ \ odot $ stars的氢膜底部两次，并通过辐射流体动力学模拟代码计算了时间演变。我们没有处理能源的起源，而是集中在单个大型恒星的重复质量爆发的动力学上。在亮度和颜色方面，第一和第二质量喷发之间存在显着差异。第二次喷发导致红色爆发事件，其中相关的亮阶段的持续时间比第一个爆发更长。即使在第一个和第二个事件中使用相同的沉积能量，弹出物质的量也不同，但差异取决于恒星的密度结构。即将进行的高节奏和深度瞬态调查将为我们提供许多前苏佩诺诺娃的活动，其中一些活动可能显示出多峰的光曲线。应解释这些因素，以考虑到密度结构的效果，并考虑到之前的爆发事件改变。
Some massive stars experience episodic and intense mass loss phases with fluctuations in the luminosity. Ejected material forms circumstellar matter around the star, and the subsequent core collapse results in a Type IIn supernova that is characterized by interaction between supernova ejecta and circumstellar matter. The energy source that triggers these mass eruptions and dynamics of the outflow have not been clearly explained. Moreover, the mass eruption itself can alter the density structure of the envelope and affect the dynamics of the subsequent mass eruption if these events are repeated. A large amount of observational evidence suggests multiple mass eruptions prior to core collapse. We investigate the density structure of the envelope altered by the first mass eruption and the nature of the subsequent second mass eruption event in comparison with the first event. We deposited extra energy at the bottom of the hydrogen envelope of 15$M_\odot$ stars twice and calculated the time evolution by radiation hydrodynamical simulation code. We did not deal with the origin of the energy source, but focused on the dynamics of repeated mass eruptions from a single massive star. There are significant differences between the first and second mass eruptions in terms of the luminosity and the color. The second eruption leads to a redder burst event in which the associated brightening phase lasts longer than the first. The amount of ejected matter is different even with the same deposited energy in the first and second event, but the difference depends on the density structure of the star. Upcoming high cadence and deep transient surveys will provide us a lot of pre-supernova activities, and some of which might show multi-peaked light curves. These should be interpreted taking the effect of density structure altered by the preceding outburst events into consideration.
