论文标题
大麦芽云中SGR 0526-66的静态硬X射线排放的Nustar检测
NuSTAR Detection of Quiescent Hard X-Ray Emission from SGR 0526-66 in the Large Magellanic Cloud
论文作者
论文摘要
软伽玛射线中继器（SGR）0526-66是第一个识别的磁铁，在大麦芽云中投影在超新星残留N49中。基于我们约50 kS的观察，我们在10-40 KEV频段中首次检测到静态状态0526-66。基于对我们的Nustar和档案Chandra ACI数据的联合分析，除了热发射外，我们还牢固地确定了0526-66的X射线频谱中非热成分的存在。在最合适的黑体（BB）加功率定律（PL）模型中，PL组件的斜率（光子指数伽马= 2.1）比其他磁铁的斜率（伽马> 〜1.5）陡峭。 X射线光谱的软部分可以用BB组件描述，温度为KT = 0.43 keV。 X射线发射区域的最佳拟合半径（r = 6.5 km）小于中子星的规范尺寸。如果我们假设中子星的典型半径为r = 10 km的基础凉爽的BB组件，除了热BB组件（2BB + PL模型）外，还可以为无源冷却中子恒星的kt = 0.24 keV获得较低的Bb温度，而kt的中子则是kt ssss的，而kt = 0.46 kt = 0.46 kt lumv specter septrim seption（lumv spection）的热点（ 0.5-5 kev频段）。仍然需要非热组件（γ〜1.8）。
The soft gamma-ray repeater (SGR) 0526-66 is the first-identified magnetar, and is projected within the supernova remnant N49 in the Large Magellanic Cloud. Based on our ~50 ks NuSTAR observation, we detect the quiescent-state 0526-66 for the first time in the 10-40 keV band. Based on the joint analysis of our NuSTAR and the archival Chandra ACIS data, we firmly establish the presence of the nonthermal component in the X-ray spectrum of 0526-66 in addition to the thermal emission. In the best-fit blackbody (BB) plus power law (PL) model, the slope of the PL component (photon index Gamma = 2.1) is steeper than those (Gamma > ~1.5) for other magnetars. The soft part of the X-ray spectrum can be described with a BB component with the temperature of kT = 0.43 keV. The best-fit radius (R = 6.5 km) of the X-ray-emitting area is smaller than the canonical size of a neutron star. If we assume an underlying cool BB component with the canonical radius of R = 10 km for the neutron star in addition to the hot BB component (2BB + PL model), a lower BB temperature of kT = 0.24 keV is obtained for the passively cooling neutron star'ssurface, while the hot spot emission with kT = 0.46 keV dominates the thermal spectrum (~85% of the thermal luminosity in the 0.5-5 keV band). The nonthermal component (Gamma ~ 1.8) is still required.
