发表机构
National Tsing Hua University; National Astronomical Observatories, CAS; Louisiana State University（国立清华大学; 中国科学院国家天文台; 路易斯安那州立大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用pGMCA获取的第谷超新星遗迹非热X射线流量图像，采用两点相关法推导磁能谱，结合X射线边缘厚度估算，发现其湍流尺度短于射电观测结果，为理解宇宙线加速提供了关键观测依据。
AI 中文摘要
超新星遗迹（SNR）被广泛认为是银河系宇宙线加速的主要来源，粒子通过扩散激波加速（DSA）机制在超新星遗迹的激波前沿获得能量，该机制使粒子通过反复穿越激波实现能量提升。磁湍流在来回散射这些粒子方面发挥着关键作用，因此对湍流的研究对于理解加速过程至关重要。在本研究中，我们应用两点相关法，从基于泊松分布的广义形态分量分析（pGMCA）获取的第谷超新星遗迹的非热X射线流量图像中推导磁能谱。所得谱中观测到的湍流长度尺度短于先前对第谷超新星遗迹射电观测研究得出的湍流尺度。此外，我们利用跨第谷超新星遗迹测量的X射线边缘厚度（该厚度是磁场强度的指标）来估算磁能谱，通过该方法推断出的湍流尺度与非热X射线流量分析得到的结果一致。
英文摘要
Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic cosmic ray acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration (DSA) mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the magnetic energy spectrum from the non-thermal X-ray flux image of Tycho's SNR. This image was obtained using Poissonian-based Generalized Morphological Component Analysis (pGMCA). The turbulence length scale observed in the resulting spectrum is shorter than the turbulence scale derived from previous studies of radio observations of Tycho's SNR. Additionally, we use the X-ray rim thickness measured across Tycho which is an indicator of magnetic field strength to estimate the magnetic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.
CommentsAccepted for publication in MNRAS
