AI 中文总结
对超亮 Ia 型超新星 SN 2022erq 进行光度和光谱研究，结合 H-α诊断与热光变曲线建模，重建其前身星爆炸前质量损失历史，发现最后几十年质量损失率增一个数量级，揭示其由白矮星和中等质量伴星组成且爆炸前质量损失不断增加。
AI 中文摘要
我们对超亮 Ia 型超新星 SN 2022erq 进行了光度和光谱研究。其早期光谱以铁族元素为主，中间质量特征较弱，可能表明核燃烧高效，与某些超亮 Ia 型超新星类似。窄巴尔末发射线的快速出现和持续存在，证明其与富氢星际介质长期相互作用，属于罕见的 Ia-CSM 类。SN 2022erq 的峰值热光度约为 8×10^43 尔格/秒，峰值后下降异常缓慢，光变曲线受长时间抛射物与星际介质相互作用主导。通过结合 H-α诊断和热光变曲线建模，重建了前身星的爆炸前质量损失历史。在最后几十年里，质量损失率增加了一个数量级，从每年约 0.04 个太阳质量增至约 0.6 个太阳质量。这一激增产生了一个约 3 个太阳质量、延伸至约 3.5×10^16 厘米的巨大星际介质壳。年轻的恒星环境（约 100 百万年）和大量的星际介质表明，前身星系统由一颗白矮星和一个中等质量伴星组成，在爆炸前质量损失不断增加。
英文摘要
We present a photometric and spectroscopic study of the superluminous Type Ia supernova SN 2022erq. Its early spectra, dominated by iron-group elements with weak intermediate-mass features, might indicate highly efficient nuclear burning, broadly similar to that inferred for some overluminous SNe Ia. The rapid emergence and persistence of narrow Balmer emission lines superposed on this iron-rich spectrum provide clear evidence of long-lived interaction with a hydrogen-rich circumstellar medium (CSM), establishing SN 2022erq as a member of the rare Ia-CSM class. SN 2022erq reached a peak bolometric luminosity of about 8 x 10^43 erg/s and exhibited an exceptionally slow post-peak decline, indicating that its light curve is dominated by long-duration ejecta-CSM interaction. By combining H-alpha diagnostics with bolometric light-curve modeling, we reconstruct the pre-explosion mass-loss history of the progenitor. The mass-loss rate escalated by one order of magnitude over the final decades, rising from about 0.04 to about 0.6 solar masses per year. This surge produced a massive, extended CSM shell of about 3 solar masses out to about 3.5 x 10^16 cm. The young stellar environment (about 100 Myr) together with this substantial, extensive CSM points to a progenitor system consisting of a white dwarf and an intermediate-mass companion that underwent increasing mass loss prior to explosion.
Comments28 pages, 18 figures, accepted for publication in ApJ
