论文标题
SN 2017HCC的高分辨率光谱及其Blueshift的线轮廓来自后震荡尘埃形成
High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation
论文作者
论文摘要
SN2017HCC是在附近且极化的超浮动型超新星（SN）方面出色的。我们获得了高分辨率的梯形光谱，并与其他光谱结合使用，以研究其线曲线的演变。所有时期都揭示了来自震动室内材料（CSM）的狭窄p〜cygni成分，表明从40-50 km/s的祖细胞出现了轴对称流出。中间宽度和宽阔的成分在发光的SNE〜IIN：对称的Lorentzian概况中显示出经典的演化，这些剖面是从早期电子散射宽扩大的震动前CSM线，在晚期过渡到多组分，从SN SN EXTEA和Shock Shock shell带来了不规则的特征。与许多SNE〜IIN一样，轮廓显示出逐渐增加的Blueshift，并且在200次又一次的中间和广泛的速度组件的红色翅膀上存在明显的通量不足。这种蓝调在连续的亮度逐渐淡出之后逐渐逐渐淡出，并且在中间延误的成分中持续了较晚的时间。在SN2017HCC中，BlueShift无法通过SN Photosphere，CSM的预击加速度或偏斜的爆炸或CSM来解释为掩盖。取而代之的是，蓝光是由后震动外壳和SN弹出中的灰尘形成产生的。该作用具有灰尘的波长依赖性，表现出与大晶粒一致的灭绝定律。因此，SN2017HCC经历了震颤后尘埃形成，并且具有轻度的双极CSM壳，类似于SN2010JL。像其他超级sneiin一样，由于十年来爆炸前的十年极端爆发的质量损失，祖先损失了10msun。
SN2017hcc was remarkable for being a nearby and strongly polarized superluminous TypeIIn supernova (SN). We obtained high-resolution echelle spectra that we combine with other spectra to investigate its line profile evolution. All epochs reveal narrow P~Cygni components from pre-shock circumstellar material (CSM), indicating an axisymmetric outflow from the progenitor of 40-50 km/s. Intermediate-width and broad components exhibit the classic evolution seen in luminous SNe~IIn: symmetric Lorentzian profiles from pre-shock CSM lines broadened by electron scattering at early times, transitioning at late times to multi-component, irregular profiles coming from the SN ejecta and post-shock shell. As in many SNe~IIn, profiles show a progressively increasing blueshift, with a clear flux deficit in red wings of the intermediate and broad velocity components after day 200. This blueshift develops after the continuum luminosity fades, and in the intermediate-width component, persists at late times even after the SN ejecta fade. In SN2017hcc, the blueshift cannot be explained as occultation by the SN photosphere, pre-shock acceleration of CSM, or a lopsided explosion or CSM. Instead, the blueshift arises from dust formation in the post-shock shell and in the SN ejecta. The effect has a wavelength dependence characteristic of dust, exhibiting an extinction law consistent with large grains. Thus, SN2017hcc experienced post-shock dust formation and had a mildly bipolar CSM shell, similar to SN2010jl. Like other superluminous SNeIIn, the progenitor lost around 10Msun due to extreme eruptive mass loss in the decade before exploding.
