Hydrogen-Rich Core-Collapse Supernovae
Hydrogen-Rich Core-Collapse Supernovae
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DOI：
10.1007/978-3-319-21846-5_39
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发表时间：
2017-10
期刊：
影响因子：
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通讯作者：
I. Arcavi
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文献类型：
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作者：
I. Arcavi
富氢核心坍缩超新星，被称为“II型”超新星，是自然界中最常见的恒星爆炸类型。它们的光谱中有明显的氢谱线。II型超新星只在恒星形成的星系中被观察到，有几个事件与大质量恒星的祖先直接相关。可以确定五个主要的亚类：IIP型（光曲线呈平台型）、IIL型（光曲线呈衰减型）、IIn型（发射线窄）、IIb型（随着时间的推移，He特征越来越强）和87a型（类似SN 1987A的光曲线呈长时间上升）。IIP型超新星已经被确定为红超巨星的爆炸，而IIL型超新星的前身仍然难以捉摸。IIn型恒星可能与明亮的蓝色变星有关，IIb型恒星的前身可能是相互作用的双星系统，而87a类恒星的原型被观测到是一颗蓝超巨星的爆炸。起源质量、金属丰度、二元性和旋转的多样性可能是观测到的爆炸类型的多样性的原因，但是起源参数和超新星性质之间的联系在理论上还没有完全理解，在观测上也没有完全映射。目前正在实施限制这种联系的新观测方法，包括对事件的大样本进行分析，利用非常早期的数据（从爆炸数小时到数天获得）和对宿主星系特性的统计研究。
Hydrogen-rich core collapse supernovae, known as "Type II" supernovae, are the most common type of stellar explosion realized in nature. They are defined by the presence of prominent hydrogen lines in their spectra. Type II supernovae are observed only in star-forming galaxies, and several events have been directly linked to massive star progenitors. Five main subclasses are identified: Type IIP (displaying a plateau in their light curve), Type IIL (displaying a light curve decline), Type IIn (displaying narrow emission lines), Type IIb (displaying increasingly strong He features with time) and 87A-likes (displaying long-rising light curves similar to that of SN 1987A). Type IIP supernovae have been robustly established as the explosions of red supergiants, while the progenitors of Type IIL's remain elusive. Type IIn's are likely linked to luminous blue variables, Type IIb progenitors may be interacting binary systems and the prototype of the 87A-like class was observed to be the explosion of a blue supergiant. The diversity in progenitor mass, metallicity, binarity and rotation is likely responsible for the diversity in observed explosion types, but the connection between progenitor parameters and supernova properties is not yet entirely understood theoretically nor fully mapped observationally. New observational methods for constraining this connection are currently being implemented, including the analyses of large samples of events, making use of very early data (obtained hours to days from explosion) and statistical studies of host-galaxy properties.