AI 中文总结
通过MUSE积分场光谱学研究SNR 0509-67.5的反向激波抛射物，发现其存在团块状结构，揭示铁电离态与速度宽度的关系，结合D6三维模型得出团块由瑞利-泰勒不稳定性导致。
AI 中文摘要
我们通过对SNR 0509-67.5的深MUSE观测中多条微弱且宽的禁线日冕发射线，报告了在该超新星遗迹的反向激波抛射物中发现了空间分辨的团块状抛射物结构。我们还在该遗迹中识别出两条此前未报道过的宽日冕发射线：[Fe xi] 7894埃和[Fe x] 6374.5埃，这扩展了此前已报道的[Fe xv] 7059.59埃、[Fe xiv] 5302.86埃、[Fe ix] 8236.55埃、[Ca xv] 5695埃以及[S xii] 7611.0埃的发射线集合。铁的近连续电离态使我们能够追踪反向激波后的电离进程。我们使用一维分析模型来模拟铁电荷态在反向激波相互作用后的演化，并将其与观测结果进行比较，结果表明需要存在激波前的团块或过密区，才能重现观测到的[Fe xiv]线表面亮度。此外，我们报告了抛射物团块的空间分辨分布，并显示反向激波相互作用会导致这些团块被压缩和碎裂。我们还发现了一个清晰的趋势：速度宽度随铁电离态的升高而减小，从最宽的[Fe ix]发射线到最窄的[Fe xv]，中间电离态物种（[Fe x]、[Fe xi]、[Fe xiv]）呈现出中间宽度。最后，我们将观测结果与具有相似铁和硫电离态的动力学驱动的双简并双星爆轰（D6）三维遗迹模型进行比较，得出观测到的团块主要由瑞利-泰勒不稳定性导致的结论。
英文摘要
We report the discovery of a spatially resolved clumpy ejecta structure in the reverse-shocked ejecta of SNR 0509-67.5, revealed through multiple faint and broad forbidden coronal emission lines in deep MUSE observations. We also identify two new broad coronal emission lines not reported before in this remnant, [Fe xi] 7894 A and [Fe x] 6374.5 A , which extend the set of previously reported [Fe xv] 7059.59 A, [Fe xiv] 5302.86 A , [Fe ix] 8236.55 A , [Ca xv] 5695 A, and [S xii] 7611.0 A. Near-continuous ionisation states of Fe allow us to follow the ionisation progression behind the reverse shock. We use a 1D analytical model to evolve Fe charge states following reverse shock interaction to compare with observations, indicating the need for preshock clumping or over-density in order to reproduce the observed surface brightness of the [Fe xiv] line. Additionally, we report the spatially resolved distribution of ejecta clumps and show that reverse-shock interaction drives their compression and fragmentation. We also find a clear trend of decreasing velocity width with increasing Fe ionisation state, from the broadest [Fe ix] emission to the narrowest [Fe xv], with intermediate-ionisation species ([Fe x], [Fe xi], [Fe xiv]) showing intermediate widths. Finally, we compare our observations to a dynamically driven double-degenerate double detonation (D6) 3D remnant model at similar Fe and S ionisation states and conclude that the observed clumps are predominantly due to Rayleigh-Taylor instabilities.
Comments15 pages, 8 figures, 3 tables
Journal refPASA, 2026;43:e105
