Abstract

I explore the origin of an asymmetry of the H\(\alpha\) emission from a circumstellar (CS) shell around type IIP supernova SN 2013fs in the spectrum taken 10.3 h after the shock breakout. A spherical model of the H\(\alpha\) emission from the CS shell that takes into account a preshock gas acceleration by a supernova radiation permits us to successfully reproduce the H\(\alpha\) profile. Principal factors responsible for the H\(\alpha\) asymmetry are the high velocity of the accelerated CS preshock gas (\({\sim}3000\) km s\({}^{-1}\)) and a low H\(\alpha\) Sobolev optical depth in a combination with an occultation of the H\(\alpha\) emission by the photosphere.

中文翻译：

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IIP型超新星SN 2013fs的第一天：来自Preshock加速气体的H $$ \ alpha $$

摘要

我探索了 在冲击爆发后10.3 h拍摄的IIP型超新星SN 2013fs周围的圆星（CS）壳H \（\ alpha \）发射的不对称起源。 考虑到超新星辐射对震前气体的加速作用，CS壳发射的H \（\ alpha \）的球形模型使我们能够成功地再现H \（\ alpha \） 轮廓。造成H \（\ alpha \） 不对称的主要因素是加速CS前冲击气的高速度（\（{\ sim} 3000 \） km s \（{} ^ {-1} \）） H \（\ alpha \）  Sobolev光学深度结合H \（\ alpha \）的掩星 由光球发射。