SN 2009kf is an exceptionally bright Type IIP Supernova (SN IIP) discovered by the Pan-STARRS 1 survey. The $V$-band magnitude at the plateau phase is $M_{V} = -18.4$ mag, which is much brighter than typical SNe IIP. We propose that its unusual properties can be naturally explained, if we assume that there was an super-Eddington energy injection into the envelope in the last few years of the evolution before the SN explosion. Using a progenitor model with such an pre-SN energy injection, we can fit the observational data of SN 2009kf with the reasonable explosion energy of $E_{\mathrm{exp}} = 2.8 \times 10^{51}$ erg and the $^{56}$Ni mass of $0.25 M_{\odot}$. Specifically, we injected the energy into the envelope at a constant rate of $3.0 \times 10^{39}$ erg s$^{-1}$ in the last 3.0 years of evolution before the core collapse. We propose that some of the unusually bright SNe IIP might result from the pre-SN energy injection to the envelope.

中文翻译：

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超新星前活动作为对 IIP 型超新星 2009kf 特殊性质的可能解释

SN 2009kf 是 Pan-STARRS 1 巡天发现的一颗异常明亮的 IIP 型超新星 (SN IIP)。平台阶段的 $V$ 波段震级为 $M_{V} = -18.4$ mag，比典型的 SNe IIP 亮得多。我们认为，如果我们假设在 SN 爆炸之前的最后几年演化过程中存在超爱丁顿能量注入包层，那么可以自然地解释其不寻常的特性。使用具有这种超前能量注入的前身模型，我们可以将 SN 2009kf 的观测数据与合理的爆炸能量 $E_{\mathrm{exp}} = 2.8 \times 10^{51}$ erg 和$^{56}$Ni 质量为 $0.25 M_{\odot}$。具体来说，我们在核心崩溃之前的最后 3.0 年的演化过程中，以 3.0 美元 \times 10^{39}$ erg s$^{-1}$ 的恒定速率将能量注入信封。