标题： 红超巨星作为超新星前身星 显示英文标题

标题： Red Supergiants as Supernova Progenitors

摘要： 大质量恒星在初始质量范围约8--30 M_{太阳}的红超巨星（RSG）阶段的不可避免命运是核心坍缩超新星（SN）爆炸，尽管一些恒星可能直接坍缩成黑洞。我们知道这是事实，因为RSGs已经在爆发前档案中的光学和红外图像中被直接识别和表征。RSGs很可能都有一些围绕恒星的物质（CSM），通过名义上的质量损失，尽管有证据表明一些RSGs在其生命周期中必须经历增强的质量损失。来自RSGs的超新星是富含氢的II型平台（II-P）超新星，光度范围低端的II-P型超新星往往来自低光度的RSGs。这种RSGs的典型光谱能量分布（SED）通常可以用一个冷光球模型来拟合，而更明亮的II-P型超新星的RSG前身星则往往需要更多的尘埃存在于其CSM中以解释它们的SED。II-P型超新星前身星的光度范围是log(L_{bol}/L_{太阳}) ~ 4.0--5.2。已知RSGs的光度达到log(L_{bol}/L_{太阳}) ~ 5.7的事实导致了所谓的“RSG问题”，这最终可能是因为到目前为止可用统计数据的数量太少。 显示英文摘要

摘要： The inevitable fate of massive stars in the initial mass range of ~8--30 M_{Sun} in the red supergiant (RSG) phase is a core-collapse supernova (SN) explosion, although some stars may collapse directly to a black hole. We know that this is the case, since RSGs have been directly identified and characterized for a number of supernovae (SNe) in pre-explosion archival optical and infrared images. RSGs likely all have some amount of circumstellar matter (CSM), through nominal mass loss, although evidence exists that some RSGs must experience enhanced mass loss during their lifetimes. The SNe from RSGs are hydrogen-rich Type II-Plateau (II-P), and SNe II-P at the low end of the luminosity range tend to arise from low-luminosity RSGs. The typical spectral energy distribution (SED) for such RSGs can generally be fit with a cool photospheric model, whereas the more luminous RSG progenitors of more luminous SNe II-P tend to require a greater quantity of dust in their CSM to account for their SEDs. The SN II-P progenitor luminosity range is log(L_{bol}/L_{Sun}) ~ 4.0--5.2. The fact RSGs are known up to log(L_{bol}/L_{Sun}) ~ 5.7 leads to the so-called ``RSG problem'', which may, in the end, be a result of small number of available statistics to date.