论文标题
发光II型短式超新星2006y，2006ai和2016EGZ：来自剥离的大型红色超级巨人的过渡类别
Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants
论文作者
论文摘要
II型超新星（SNE II）的多样性被认为主要是由于其祖细胞丰富（富含H的）包膜质量的差异，而Sne IIP具有长高原（$ \ sim100 $天）和最庞大的H-富含H-富含H-富含H的包裹。但是，这是一个持续的谜，为什么很少见到短高原（数十天）的Sne II。在这里，我们介绍了发光的II型短款Short-Plateau Sne Sne 2006y，2006AI和2016EGZ的光学/近红外光度和光谱观察结果。他们的高原约为50美元 - $ 70 $天，并发光光学峰（$ \ Lesssim-18.4 $ mag）表明明显的前探索质量损失，导致部分剥离的H丰富的Hemperion和早期的异形材料（CSM）相互作用。我们计算了具有各种祖细胞零老年序列（ZAMS）质量，质量损失效率，爆炸能，$^{56} $ ni质量和CSM肿块和CSM浓度的大量梅萨+Stella单星祖细胞和光曲线模型。我们的模型网格显示了在富含H的包膜质量下降顺序中连续的SNE IIP-IIL-IIL-IIB样光曲线形态。带有大$^{56} $ ni masses（$ \ gtrsim0.05 \，m_ \ odot $），Short-plateau sne ii位于狭窄的参数空间中，作为SNE IIL和IIB之间的过渡类别。对于Sne 2006y，2006AI和2016EGZ，我们的发现表明高质量红色超级巨人（RSG）祖先（$ M _ {\ rm Zams} \ Simeq 18 $ - $ 22 \，M _ {\ odot} $），带有小型H-含H-含H-含H-含H-含H-含H-含量的内心（$ M _）（$ m _} \ simeq 1.7 \，m _ {\ odot} $）在上一位前几年之前经历了增强的质量损失（$ \ dot {m} \ simeq 10^{ - 2} \，m _ {\ odot} \，{\ rm yr}^{ - rm yr}^{ - 1} $）如果高质量RSG会导致罕见的短plateau sne II，那么这些事件可能会缓解观察到的SN II祖细胞样品中较高luminusity RSG的某些明显不足。
The diversity of Type II supernovae (SNe II) is thought to be driven mainly by differences in their progenitor's hydrogen-rich (H-rich) envelope mass, with SNe IIP having long plateaus ($\sim100$ days) and the most massive H-rich envelopes. However, it is an ongoing mystery why SNe II with short plateaus (tens of days) are rarely seen. Here, we present optical/near-infrared photometric and spectroscopic observations of luminous Type II short-plateau SNe 2006Y, 2006ai, and 2016egz. Their plateaus of about $50$-$70$ days and luminous optical peaks ($\lesssim-18.4$ mag) indicate significant pre-explosion mass loss resulting in partially stripped H-rich envelopes and early circumstellar material (CSM) interaction. We compute a large grid of MESA+STELLA single-star progenitor and light-curve models with various progenitor zero-age main-sequence (ZAMS) masses, mass-loss efficiencies, explosion energies, $^{56}$Ni masses, and CSM densities. Our model grid shows a continuous population of SNe IIP-IIL-IIb-like light-curve morphology in descending order of H-rich envelope mass. With large $^{56}$Ni masses ($\gtrsim0.05\,M_\odot$), short-plateau SNe II lie in a confined parameter space as a transitional class between SNe IIL and IIb. For SNe 2006Y, 2006ai, and 2016egz, our findings suggest high-mass red supergiant (RSG) progenitors ($M_{\rm ZAMS} \simeq 18$-$22\,M_{\odot}$) with small H-rich envelope masses ($M_{\rm H_{\rm env}} \simeq 1.7\,M_{\odot}$) that have experienced enhanced mass loss ($\dot{M} \simeq 10^{-2}\,M_{\odot}\,{\rm yr}^{-1}$) for the last few decades before the explosion. If high-mass RSGs result in rare short-plateau SNe II, then these events might ease some of the apparent underrepresentation of higher-luminosity RSGs in observed SN II progenitor samples.
