发表机构
San Diego State University（圣地亚哥州立大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
研究大麦哲伦星系新星，结合Yaron等人2005年的新星模型与光变曲线数据，发现LMC新星比M31和银河系中的新星更亮且演化更快，白矮星质量和膨胀速度更高，再发新星爆发百分比也更高，未来观测或革新相关理解。
AI 中文摘要
本文对大麦哲伦星系（LMC）中的新星进行了全面研究。在过去一个世纪（1926 - 2025年），LMC共报告了66次新星爆发。其中39个独特前身系统的48次爆发（9次是4颗已知再发新星的复发）有足够光度数据来可靠估计最大星等和下降速率。这些数据证实LMC新星平均比仙女座星系（M31）或银河系中的新星更亮且演化更快。首次将Yaron等人（2005年）的新星模型与光变曲线数据结合来估计LMC新星群体的基本属性。模型表明LMC新星通常具有比M31新星更高的白矮星质量和膨胀速度，这导致LMC中再发新星爆发的百分比（约20.6%）高于M31（约6.40%）。未来维拉·鲁宾天文台的观测有望彻底改变我们对LMC及本星系群以外星系中新星群体的理解。
英文摘要
A comprehensive study of novae in the Large Magellanic Cloud (LMC) is presented. A total of 66 nova eruptions have been reported in the LMC over the past century ($1926 \unicode{x2013} 2025$). Of these, a total of 48 eruptions from 39 unique progenitor systems (nine eruptions are recurrences of four known recurrent novae) have sufficient photometric data to permit the maximum magnitudes and rates of decline to be reliably estimated. These data confirm earlier studies showing that LMC novae are, on average, slightly more luminous and faster evolving compared with novae in the Andromeda galaxy (M31) or the Milky Way. For the first time, the nova models of Yaron et al. have been used in conjunction with the light-curve data to estimate the fundamental properties of the LMC nova population. The models suggest that LMC novae are characterized by generally higher white dwarf (WD) masses and higher expansion velocities compared with M31 novae. The higher average WD masses have resulted in a higher percentage of recurrent nova eruptions in the LMC ($\sim$20.6%) compared with that seen in M31 ($\sim$6.40%). Future observations made possible by the Vera Rubin Observatory promise to revolutionize our understanding of nova populations in the LMC and in galaxies beyond the Local Group.
Comments34 pages; 6 tables; 15 figures; typos corrected; reference added; published in The Astrophysical Journal Supplement Series
Journal refAllen W. Shafter 2026 ApJS 286 31
