论文标题
Suzaku对超新星残留W51C中的Fe K-shell线的观察和近距离X射线源的观察
Suzaku Observations of Fe K-shell Lines in the Supernova Remnant W51C and Hard X-ray Sources in the Proximity
论文作者
论文摘要
在本文中，我们研究了超新星残留W51C中的Fe K-shell线，并在接近度中调查了硬新型X射线源。我们分别测量了Fe i k $α$和Fe xxv He $α$线的强度分别为6.40 KEV和6.68 KEV，发现6.68 KeV线的强度与以前的研究中预期的背景水平一致，而6.40 KEV线的强度在2.0 $ = $ = $ = $ = 0.40 KEV线的强度较高。鉴于存在伽马射线发射和高电离速率点在空间上与残留物相吻合，我们得出的结论是，增强的6.40 keV线最有可能源自低能量宇宙射线与分子云之间的相互作用。另外，我们发现了从紧凑的H II区G49.0-0.3的增强型6.68 keV线发射，显着性水平为3.4 $σ$。光谱分析表明，6.68 keV线的热等离子体的温度和丰度分别为$ kt = 3.0^{+0.8} _ { - 0.7} $ keV和$ z = 0.5 \ pm 0.2 $ solar。这些值是由O恒星恒星风产生的热等离子体来解释的。
In this paper, we investigated the Fe K-shell lines in the supernova remnant W51C and hard X-ray sources in the proximity. We measured the intensities of Fe I K$α$ and Fe XXV He$α$ lines at 6.40 keV and 6.68 keV, respectively, and found that the intensity of the 6.68 keV line is consistent with the background level expected from previous studies, while that of the 6.40 keV line is higher at the significance level of 2.0$σ$. Given the presence of gamma-ray emission and high ionization rate point spatially coincident with the remnant, we conclude that the enhanced 6.40 keV line most likely originates from the interaction between low-energy cosmic rays and molecular clouds. Also, we discovered an enhanced 6.68 keV line emission from the compact H II region G49.0-0.3 at the significance level of 3.4$σ$. Spectral analysis revealed that the temperature and abundance of the thermal plasma with the 6.68 keV line is $kT = 3.0^{+0.8}_{-0.7}$ keV and $Z = 0.5 \pm 0.2$ solar, respectively. These values are explained by the thermal plasma generated by the stellar winds of O stars.
