We present the first coordinated soft and hard 0.3–80 keV X-ray campaign of the extragalactic supernova SN2014C in the first ∼2307 days of its evolution. SN2014C initially appeared to be an ordinary type Ib explosion but evolved into a strongly-interacting hydrogen-rich SN IIn over ∼1 yr. We observed signatures of interaction with a dense medium across the X-ray spectrum, which revealed the presence of a ∼1−2M _⊙ shell of material at ∼6נ10¹⁶ cm from the progenitor. This finding challenges current understanding of hydrogen-poor core-collapse progenitor evolution. Potential scenarios to interpret these observations include (i) the ejection of the hydrogen envelope by the progenitor star in the centuries prior to the explosion; (ii) interaction of the fast Wolf-Rayet (WR) star wind with the slow, dense wind of the Red Super Giant phase, with an anomalously short WR phase.

我们介绍了银河系超新星SN2014C在演化的前2307天中首次进行的软硬0.3-80 keV协调X射线运动。SN2014C最初看起来是普通的Ib型爆炸，但在大约1年的时间内演变为强相互作用的富氢SN IIn。我们观察到相互作用的签名与整个X射线光谱的稠密介质，其揭示了~1-2的存在中号 _⊙在~6נ10材料的外壳¹⁶ 距祖细胞厘米。这一发现挑战了当前对贫氢核心塌陷祖细胞进化的理解。解释这些观察结果的可能情况包括：（i）爆炸前几个世纪以来，祖先恒星喷出了氢包层；（ii）沃尔夫-雷耶特（WR）快星风与红色超巨星相缓慢而密集的风以及异常短WR相的相互作用。