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arXiv 1807.09778astro-ph.SRastro-ph.HE
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闪光（超新星）光谱学的物理学

The Physics of Flash (Supernova) Spectroscopy

C. S. Kochanek

备注：
12 pages, 8 figures, submitted to MNRAS
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摘要：

我们研究了由超新星（SN）的新兴冲击波产生的硬辐射脉冲电离的星周介质（CSM）的闪光光谱。我们首先发现，对于半径为Rstar且冲击速度为vshock的恒星，Halpha发射的上升和下降时间限制了CSM的位置，峰值位于tpeak=Rstar sqrt（2/c vshock）。瞬态发射温度的下降自然地再现了具有不同电离能的谱线的演化。其次，对于红超巨星（RSG），激波爆发辐射加速CSM产生广泛的，早期的线翼独立的汤姆逊光学深度的CSM。最后，CSM复合率在二进制可以占主导地位的密集，凉爽，风碰撞界面，如沃尔夫-拉叶二进制，而不是个人的恒星风。结合这三个结果，正常的IIP型iPTF 13 dqy（SN 2013 fs）的闪光光谱观测结果自然可以用一个RSG来解释，该RSG具有正常的汤姆逊光学薄风，在一个双星中，分离度为~10^4 Rsun，而不需要任何SN前的爆发。类似地，IIb型iPTF 13 ast（SN 2013 cu）的宽线翼，其前身通常是双星中的黄超巨星，可能是由于CSM的辐射加速，而不是预先存在的沃尔夫-拉叶风。

英文摘要：

We examine flash spectroscopy of a circumstellar medium (CSM) ionized by the hard radiation pulse produced by the emerging shock of a supernova (SN). We first find that the rise and fall times of the Halpha emission constrains the location of the CSM with a peak at tpeak=Rstar sqrt(2/c vshock) for a star of radius Rstar and a shock velocity of vshock. The dropping temperature of the transient emission naturally reproduces the evolution of lines with different ionization energies. Second, for red supergiants (RSGs), the shock break out radiatively accelerates the CSM to produce broad, early-time line wings independent of the Thomson optical depth of the CSM. Finally, the CSM recombination rates in binaries can be dominated by a dense, cool, wind collision interface like those seen in Wolf-Rayet binaries rather than the individual stellar winds. Combining these three results, the flash spectroscopy observations of the normal Type IIP iPTF13dqy (SN 2013fs) are naturally explained by an RSG with a normal, Thomson optically thin wind in a binary with a separation of ~10^4 Rsun without any need for a pre-SN eruption. Similarly, the broad line wings seen for the Type IIb iPTF13ast (SN 2013cu), whose progenitors are generally yellow supergiants in binaries, are likely due to radiative acceleration of the CSM rather than pre-existing, Wolf-Rayet-like wind.

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