标题： 具有旋转的对 Instability 超新星的发射 显示英文标题

标题： Emission from Pair-Instability Supernovae with Rotation

摘要： 对一些超亮超新星（例如SN 2007bi）以及早期宇宙中由大质量、零金属度的第三族恒星爆发产生的主要爆炸类型之一，脉冲不稳定超新星曾被认为是候选者。 此类事件的前身星可能是快速旋转的，因此由于旋转引起的混合和质量损失效应表现出不同的演化特性。 准确识别这些事件需要严格的辐射流体力学和辐射传递计算，不仅要捕捉光变曲线的行为，还要捕捉这些事件的光谱演化。 我们展示了覆盖激波突破和晚期光变曲线阶段的90至300倍太阳质量旋转脉冲不稳定超新星的辐射流体力学和辐射传输计算。 我们还研究了不同初始金属丰度和旋转速率的情况，以确定这些参数对这些事件详细光谱特征的影响。 与最近关于非旋转脉冲不稳定超新星的结果一致，我们发现，在一定范围的前身星质量和旋转速率下，这些事件具有本质上偏红的颜色，这与超亮超新星的观测结果相矛盾。 旋转脉冲不稳定超新星的光谱特性与剥离氢和氦包层的非旋转事件相似。 我们发现，前身星的金属丰度和旋转速率特性在爆炸后会被抹去，在最终模型光谱中无法识别。 超新星爆炸前的质量损失以及超新星喷出物的基本属性（如质量、温度和速度）对脉冲不稳定超新星的模型光谱有最直接的影响。 显示英文摘要

摘要： Pair Instability Supernovae have been suggested as candidates for some Super Luminous Supernovae, such as SN 2007bi, and as one of the dominant types of explosion occurring in the early Universe from massive, zero-metallicity Population III stars. The progenitors of such events can be rapidly rotating, therefore exhibiting different evolutionary properties due to the effects of rotationally-induced mixing and mass-loss. Proper identification of such events requires rigorous radiation hydrodynamics and radiative transfer calculations that capture not only the behavior of the light curve but also the spectral evolution of these events. We present radiation hydrodynamics and radiation transport calculations for 90-300 Msun rotating pair-instability supernovae covering both the shock break-out and late light curve phases. We also investigate cases of different initial metallicity and rotation rate to determine the impact of these parameters on the detailed spectral characteristics of these events. In agreement with recent results on non-rotating pair instability supernovae, we find that for a range of progenitor masses and rotation rates these events have intrinsically red colors in contradiction with observations of super-luminous supernovae. The spectroscopic properties of rotating pair instability supernovae are similar to those of non-rotating events with stripped hydrogen and helium envelopes. We find that the progenitor metallicity and rotation rate properties are erased after the explosion and cannot be identified in the resulting model spectra. It is the combined effects of pre-supernova mass-loss and the basic properties of the supernova ejecta such as mass, temperature and velocity that have the most direct impact in the model spectra of pair instability supernovae.