发表机构
University of Manitoba; Los Alamos National Laboratory; The George Washington University（曼尼托巴大学; 洛斯阿拉莫斯国家实验室; 乔治华盛顿大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过多波段观测分析超新星遗迹MSH 15-52，揭示其壳层结构、喷流与超新星遗迹的相互作用，为探究脉冲星-PWN-SNR相互作用提供了重要观测依据。
AI 中文摘要
我们利用钱德拉（Chandra）、XMM-牛顿（XMM-Newton）和eROSITA望远镜，结合MeerKAT射电数据，对与年轻旋转驱动脉冲星PSR B1509-52相关的超新星遗迹（SNR）MSH 15-52开展X射线分析。我们报告发现了明亮的北部RCW 89区域缺失的南部对应体，并识别出一个可能为此前未确认的SNR候选体的前景X射线源。XMM-牛顿和eROSITA的成像与光谱分析揭示了MSH 15-52的壳层特性，表明其南部和北部的类壳结构均与前激波相关的受激星际介质一致，而它们的低电离时标及可能的硬幂律成分，暗示可能受到脉冲星风云（PWN）喷流的粒子注入或额外加热的影响。钱德拉对南部喷流的新光谱图显示出一个硬非热辐射区域，其光子指数约为1.6，表明PWN与反向激波之间存在相互作用，且可能存在脉冲星外流的再加速。对RCW 89北部团块的空间分辨光谱分析揭示了富含金属的高速抛射物，其Ne和Mg丰度增强。与核心坍缩核合成模型的比较显示，一维产额模型支持初始质量约为29倍太阳质量的大质量前身星，而不对称爆炸模型表明较低质量的前身星也能重现观测到的丰度比。我们的研究支持如下图景：RCW 89是与高能脉冲星喷流相互作用的更大不对称SNR壳层的一部分，使该系统成为探究脉冲星-PWN-SNR相互作用的宝贵实验室。
英文摘要
We present an X-ray analysis of the supernova remnant (SNR) MSH 15-52 associated with the young rotation-powered pulsar PSR B1509-58, using Chandra, XMM-Newton, and eROSITA, complemented by MeerKAT radio data. We report the discovery of the missing southern counterpart to the bright northern RCW 89 region and identify a foreground X-ray source that may be a previously unidentified SNR candidate. Imaging and spectroscopy with XMM-Newton and eROSITA reveal the shell properties of MSH 15-52 and suggest that both the southern and northern shell-like structures are consistent with shocked interstellar medium associated with the forward shock, while their low ionization timescales and possible hard power-law components indicate possible influence from particle injection or additional heating by the pulsar wind nebula (PWN) jets. New Chandra spectral maps of the southern jet reveal a region of hard non-thermal emission, with a photon index of approximately 1.6, suggesting interaction between the PWN and the reverse shock and possible re-acceleration of the pulsar outflow. Spatially resolved spectroscopy of the RCW 89 northern clumps reveals high-velocity, metal-rich ejecta with enhanced Ne and Mg abundances. Comparison with core-collapse nucleosynthesis models favors a massive progenitor with an initial mass of approximately 29 solar masses in one-dimensional yield models, while asymmetric explosion models show that lower-mass progenitors can also reproduce the observed abundance ratios. Our study supports a picture in which RCW 89 is part of a larger asymmetric SNR shell interacting with energetic pulsar jets, making the system a valuable laboratory for probing pulsar-PWN-SNR interaction.
Comments21 pages, 17 figures. Accepted for publication in The Astrophysical Journal
