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arXiv 2003.02709astro-ph.HE
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宽线Ic型超新星ASASSN-16 fp的射电图像

Radio view of a broad-line Type Ic supernova ASASSN-16fp

Nayana A. J., Poonam Chandra

备注：
14 pages, 7 figures, Accepted for publication in MNRAS
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摘要：

我们提出了广泛的无线电观测的Ic型超新星，ASASSN-16 fp。我们的数据代表的SN超过1000天的最低频率的观测与频率范围的$0.33-25$ GHz和时间范围的$\sim$ 8至1136天后爆炸。观测结果最好由一个模型的同步辐射从一个冲击拱壳最初抑制同步自吸收。假设相对论粒子和磁场能量均分，在爆炸后第8天的$t_{0}$ $\sim$上，我们估计爆炸波的速度和半径分别为$v \sim 0.15c$和$r \sim 3.4$ $\times$ $10^{15}$ cm。我们推断放射性物质的总内能演化为$E$ $\sim$ 0.37 $\times$ $10^{47}$（t/t $_{0}$）$^{0.65}$ erg。我们确定的质量损失率的祖星$\dot{M}$ $\sim$ $(0.4-3.2) \times10^{-5}$ $M_{\odot}\rm yr^{-1}$在爆炸后的各个时期，与银河系沃尔夫-拉叶星的质量损失率一致。射电光变曲线和光谱表明，在距离爆炸中心半径为$\sim$ $1.10 \times 10^{16}$ cm的CSM中存在密度增强的特征。

英文摘要：

We present extensive radio observations of a Type Ic supernova, ASASSN-16fp. Our data represents the lowest frequency observations of the SN beyond 1000 days with a frequency range of $0.33-25$ GHz and a temporal range of $\sim$ 8 to 1136 days post-explosion. The observations are best represented by a model of synchrotron emission from a shocked circumstellar shell initially suppressed by synchrotron self-absorption. Assuming equipartition of energy between relativistic particles and magnetic fields, we estimate the velocity and radius of the blast wave to be $v \sim 0.15c$ and $r \sim 3.4$ $\times$ $10^{15}$ cm respectively at $t_{0}$ $\sim$ 8 days post-explosion. We infer the total internal energy of the radio-emitting material evolves as $E$ $\sim$ 0.37 $\times$ $10^{47}$ (t/t$_{0}$)$^{0.65}$ erg. We determine the mass-loss rate of the progenitor star to be $\dot{M}$ $\sim$ $(0.4-3.2) \times10^{-5}$ $M_{\odot}\rm yr^{-1}$ at various epochs post-explosion, consistent with the mass-loss rate of Galactic Wolf-Rayet stars. The radio light curves and spectra show a signature of density enhancement in the CSM at a radius of $\sim$ $1.10 \times 10^{16}$ cm from the explosion center.

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