超亮超新星2018ibb中的主要与次要能量来源
Primary and secondary source of energy in the superluminous supernova 2018ibb
AI总结：
本文通过对超亮超新星2018ibb进行对不稳定性超新星建模与辐射转移模拟，提出含34倍太阳质量56Ni的模型可解释其主要光变与光谱特征，并用星周物质相互作用解释观测到的额外能量来源。
摘要：
我们研究了超亮超新星2018ibb的对不稳定性起源。作为基础模型，我们采用一个初始质量为250倍太阳质量、金属丰度约为太阳金属丰度1/15的非旋转恒星模型。我们考虑该模型的三个版本作为使用STELLA和ARTIS程序进行的辐射转移模拟的输入：含25倍太阳质量的56Ni、含34倍太阳质量的56Ni，以及含34倍太阳质量的56Ni的化学混合情形。我们展示光变曲线和光谱，并与SN 2018ibb的观测数据进行比较，得出结论：含34倍太阳质量的56Ni的对不稳定性超新星模型能够合理地解释峰值前后-100天至250天之间的宽波段光变曲线。我们的合成光谱与观测光谱有许多相似之处。光变曲线中的光度超出和光谱中的蓝端流量超出可以由一个额外的能量来源解释，该来源可能是超新星抛射物与 circumstellar matter（星周物质）的相互作用。我们讨论了在对不稳定性爆炸之前几十年内被抛射出的星周物质起源的可能机制。
英文摘要：
We examine the pair-instability origin of superluminous supernova 2018ibb. As the base model, we use a non-rotating stellar model with an initial mass of 250 Msun at about 1/15 solar metallicity. We consider three versions of the model as input for radiative transfer simulations done with the STELLA and ARTIS codes: with 25 Msun of 56Ni, 34 Msun of 56Ni, and a chemically mixed case with 34 Msun of 56Ni. We present light curves and spectra in comparison to the observed data of SN 2018ibb, and conclude that the pair-instability supernova model with 34 Msun of 56Ni explains broad-band light curves reasonably well between -100 and 250 days around the peak. Our synthetic spectra have many similarities with the observed spectra. The luminosity excess in the light curves and the blue-flux excess in the spectra can be explained by an additional energy source, which may be interaction of the SN ejecta with circumstellar matter. We discuss possible mechanisms of the origin of the circumstellar matter being ejected in the decades before the pair-instability explosion.
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