NGC 6946中经典型II-P超新星2017 eaw的BVRI测光：第3天至第594天
BVRI Photometry of the Classic Type II-P Supernova 2017eaw in NGC 6946: Day 3 to Day 594
摘要：
NGC 6946中SN 2017 eaw的宽带$BVRI$光变曲线揭示了II-P型超新星的经典元素。观测于2017年5月16日（UT）开始，大约在发现宣布后1天，光度监测进行了近600天。光变曲线显示出一个明确的平台和一个指数尾部，在稍后的时间略有弯曲。近似的辐射热光变曲线的推导和用于估计的$^{56}$镍在爆炸中产生的量，从文献中描述的各种方法，我们得到$M$（$^{56}{\rm Ni}$）= 0.115（$-$ 0.022，+0.027）$M_{\odot}$。我们还估计，43%的辐射热通量发射在平台阶段实际上是由$^{56}$镍链。其他的参数支持了母星是一颗红超巨星的观点。
英文摘要：
Broadband $BVRI$ light curves of SN 2017eaw in NGC 6946 reveal the classic elements of a Type II-P supernova. The observations were begun on 16 May 2017 (UT), approximately 1 day after the discovery was announced, and the photometric monitoring was carried out over a period of nearly 600 days. The light curves show a well-defined plateau and an exponential tail which curves slightly at later times. An approximation to the bolometric light curve is derived and used to estimate the amount of $^{56}$Ni created in the explosion; from various approaches described in the literature, we obtain $M$($^{56}{\rm Ni}$) = 0.115 ($-$0.022,+0.027)$M_{\odot}$. We also estimate that 43\% of the bolometric flux emitted during the plateau phase is actually produced by the $^{56}$Ni chain. Other derived parameters support the idea that the progenitor was a red supergiant.
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