外層剝離超新星(Stripped-envelope supernovae, SE SNe)之外層剝離曾被認為是單一顆大質量恆星的強烈恆星風所造成的現象，但後續的觀測結果顯示，此種超新星更可能源自於雙星系統中雙星間的交互作用。最直接支持雙星系統來源的觀測證據，是觀測上找到此種超新星的倖存伴星，因為多個理論模擬研究已證明，超新星的伴星能夠歷經超新星爆發衝擊後仍存續，而且有機會被望遠鏡給捕捉。近期，根據哈伯太空望遠鏡(Hubble Space Telescope, HST)的光度及頻譜觀測，Gagliano等人發表了一個位於鄰近星系M100(距離約17.1百萬秒差距)的Ic型超新星SN 2020oi，並認為其源自雙星系統。根據Gagliano等人提供的SN 2020oi雙星系統性質，我們進行了超新星-伴星交互作用的二維流體力學模擬，以及受衝擊後倖存伴星之後續演化模擬。我們的結果顯示，倖存伴星在受衝擊後，亮度增加了兩個數量級，且表面頻譜暫時性的變紅(即表面溫度變低)。此伴星有機會以韋伯太空望遠鏡(James Webb Space Telescope, JWST)的近紅外相機NIRCam的短波長頻道進行偵測。此外，我們的伴星模型的相對星等在達到最大值後便產生明顯的劇降：這也許是一個分辨外層剝離超新星的倖存伴星訊號的好指標。

Stripped-envelope supernovae (SE SNe) were considered as the explosions of single massive stars with strong stellar winds, while later observations favor binary origins. One direct evidence to support the binary origins is to find the surviving companions of SE SNe since previous numerical studies suggested that the binary companion should survive the supernova impact and could be detectable. Recently, Gagliano et al. (2022) reported that the nearby Type Ic SN 2020oi in M100 (~17.1 Mpc) resulted from a binary system based on the HST photometric and spectroscopic observation. Based on the suggested binary properties of SN 2020oi, we conduct two-dimensional hydrodynamics simulations of supernova-companion interactions and the subsequent post-impact evolution of the companion. Our results suggest that a surviving companion becomes brighter in two orders of magnitude and temporarily redder after the SN impact. The companion might be detectable with the JWST NIRCam short wavelength channel in a few years. Furthermore, the predicted magnitudes of surviving companions show a significant magnitude gradient around the peak. This could be another good indicator to identify the surviving companion from a SE SN.

Abstract (Chinese) P. I
Acknowledegments (Chinese) P. II
Abstract P. III
Acknowledgements P. IV
Contents P. V
List of Figures P. VII
List of Tables P. XI
1 Background P. 1
2 Main Body P. 3
2.1 Introduction P.3
2.2 Numerical Methods P.7
2.3 Results P. 12
2.4 Discussion P. 20
3 Summary and Conclusions P. 29
4 Supplemental Materials P. 31
Bibliography P. 37

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