不安分的SN2009ip的全色图像揭示了大质量恒星包层的爆炸性喷射
A panchromatic view of the restless SN2009ip reveals the explosive ejection of a massive star envelope
摘要：
2012年SN 2009 ip的爆炸引发了我们对大质量恒星演化后期阶段的理解问题。在这里，我们提出了一个全面的研究SN 2009 ip在其显着的再增亮（S）。从GeV到射电波段的高节奏测光和光谱观测来自各种地面和空间设施（包括VLA，Swift，Fermi，HST和XMM），这些观测结果表明SN 2009 ip是一个低能量（E~ 10^50 erg，喷出物质量约为0.5 Msun），并且可能是在一个复杂介质中的不对称爆炸，该介质由不安分的祖星多次爆发形成。大部分的能量是由于冲击波通过位于5x10^14 cm处的致密物质壳层爆发而辐射出来的，该物质壳层的M约为0.1 Msun，是在大爆炸前约40天由前兆爆发喷出的。我们将近红外过量辐射解释为位于更远处（R> 4 × 10^15 cm）的物质的尘埃蒸发的特征，其起源必须与前几年记录的质量损失事件有关。我们的模型预测明亮的中微子发射与冲击波爆发，如果宇宙射线的能量是可比的辐射能量。我们将这种现象与大质量祖星外层的爆炸性喷射联系起来，后者后来与之前爆发所沉积在周围的物质相互作用。未来的观测将揭示发光蓝变星（LBV）的祖先星是否幸存下来。无论爆炸是否是终端，SN 2009 ip揭示了持续的偶发性质量损失的新渠道的存在，其物理起源尚未确定。
英文摘要：
The 2012 explosion of SN2009ip raises questions about our understanding of the late stages of massive star evolution. Here we present a comprehensive study of SN2009ip during its remarkable re-brightening(s). High-cadence photometric and spectroscopic observations from the GeV to the radio band obtained from a variety of ground-based and space facilities (including the VLA, Swift, Fermi, HST and XMM) constrain SN2009ip to be a low energy (E~ 10^50 erg for an ejecta mass ~ 0.5 Msun) and likely asymmetric explosion in a complex medium shaped by multiple eruptions of the restless progenitor star. Most of the energy is radiated as a result of the shock breaking out through a dense shell of material located at 5x10^14 cm with M~0.1 Msun, ejected by the precursor outburst ~40 days before the major explosion. We interpret the NIR excess of emission as signature of dust vaporization of material located further out (R>4x 10^15 cm), the origin of which has to be connected with documented mass loss episodes in the previous years. Our modeling predicts bright neutrino emission associated with the shock break-out if the cosmic ray energy is comparable to the radiated energy. We connect this phenomenology with the explosive ejection of the outer layers of the massive progenitor star, that later interacted with material deposited in the surroundings by previous eruptions. Future observations will reveal if the luminous blue variable (LBV) progenitor star survived. Irrespective of whether the explosion was terminal, SN2009ip brought to light the existence of new channels for sustained episodic mass-loss, the physical origin of which has yet to be identified.
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