论文标题
IPTF14HL中的IPTF14HL在情节介质相互作用模型中：脉冲配对超新星的有前途的候选者
iPTF14hls in the circumstellar medium interaction model: A promising candidate for a pulsational pair-instability supernova
论文作者
论文摘要
IPTF14HLS是一种发光的II型超新星（SN），其起源仍然存在颠簸的光曲线。自从发现大约600天以来，它具有大约恒定的有效温度和发光度，然后衰变缓慢。发现$ \ sim 1000 $ \ days发现后的光曲线过渡到非常急剧下降。在这个急剧下降阶段采取的频谱显示出与密集的偶然培养基（CSM）的冲击相互作用的明显特征。在这里，我们探讨了IPTF14HL作为相互作用的SN的可能性。 IPTF14HL的光曲线可以装有风状CSM。分析建模表明，在最后的$ \ sim 200 \ mathrm {yr} $中，IPTF14HL可能已经承担了六集的群众损失。假设1954年的喷发触发了最后的质量损失情节，则根据不同的模型，恒星速度被确定为$ 40-70 \ Mathrm {km} \ Mathrm {s}^{ - 1} $，具体取决于不同的模型。质量损失率在$％0.4-33m _ {\ odot} \ mathrm {yr}^{ - 1} $的范围内。推断的弹出总质量（$ M _ {\ Mathrm {ej}}+M _ {\ MathRm {\ MathRM {csms}} \ Simeq 245m _ {\ odot} $）支持IPTF14HLS可能是（PulSational）的观念。发现和观察更相似的恒星爆炸将有助于理解这些奇特的SNE。
iPTF14hls is a luminous Type II supernova (SN) with a bumpy light curve that remains debated for its origin. It maintains roughly a constant effective temperature and luminosity since discovery for about 600 days, followed by a slow decay. On $\sim 1000$\ days post discovery the light curve transitions to a very steep decline. A spectrum taken during this steep decline phase shows clear signatures of shock interaction with dense circumstellar medium (CSM). Here we explore the possibility of iPTF14hls as an interaction-powered SN. The light curve of iPTF14hls can be fitted with wind-like CSMs. Analytic modeling indicates that iPTF14hls may have undertaken six episodes of mass loss during the last $\sim 200\mathrm{yr}$. Assuming that the 1954 eruption triggered the last mass-loss episode, the stellar-wind velocity is determined to be $40-70\mathrm{km}\mathrm{s}^{-1}$, depending on different models. Mass loss rates are in the range $% 0.4-3.3M_{\odot }\mathrm{yr}^{-1}$. The inferred total mass of ejecta and CSMs ($M_{\mathrm{ej}}+M_{\mathrm{CSMs}}\simeq 245M_{\odot }$) supports the idea that iPTF14hls may be a candidate for a (pulsational) pair-instability SN. Discovery and observations of more similar stellar explosions will help understand these peculiar SNe.
