论文标题
银河中心的Chandra大规模映射：探测中央分子区域周围的高能结构
Chandra large-scale mapping of the Galactic center: Probing high-energy structures around the central molecular zone
论文作者
论文摘要
最近的观察结果揭示了星际特征，这些特征显然将我们星系中央区域的能量活性与光晕联系在一起。但是，这些特征的性质在很大程度上仍然不确定。我们提出了银河系中央2x4平方田场的Chandra映射，揭示了从银河系中心（GC）出现的X射线发射螺纹以及羽状样结构的复合物。该映射表明，北部的羽流或喷泉被众所周知的无线电叶（或GCL）所抵消，但是，这可能代表了前景HII地区，并且南部羽流被Meerkat最近发现的相应无线电叶所包裹。特别是，我们发现一个明显的X射线线G0.17-0.41嵌入了局部充气的非热无线电丝中。该宽度约为1.6英寸（FWHM）的线在GC的距离处长度〜6 pc，具有频谱，可以以功率定律或温度〜3 keV的光学性法律或光学薄的热等离子体为特征。X射线发出的材料可能限制在磁场内，并不限制其强度> 1 mg，无界的无限范围，这些属性是无关的，这些属性是无关的，这些杂物是这些范围的，这些均可群体和这些宽度的范围和这些范围的范围，这些频率是这些范围的范围，这些频谱和这些相关的范围和这些相关的范围和这些相关的范围和这些相关性。当磁场的重新连接是当反平行磁场的通量碰撞和/或扭曲的射击X射线羽流中，代表较年轻的大型型号的GC中的GC的理解，该磁场可能是对较年轻的大量群，这是对分析的较高的flar solog for come for solog for solog，磁场可能会在分析中，而在弥漫性的X射线羽毛中碰撞时，可能会在GC中驱动。星际热等离子体加热，宇宙射线加速度和湍流。
Recent observations have revealed interstellar features that apparently connect energetic activity in the central region of our Galaxy to its halo. The nature of these features, however, remains largely uncertain. We present a Chandra mapping of the central 2x4 square degree field of the Galaxy, revealing a complex of X-ray-emitting threads plus plume-like structures emerging from the Galactic center (GC). This mapping shows that the northern plume or fountain is offset from a well-known radio lobe (or the GCL), which however may represent a foreground HII region, and that the southern plume is well wrapped by a corresponding radio lobe recently discovered by MeerKAT. In particular, we find that a distinct X-ray thread, G0.17-0.41, is embedded well within a nonthermal radio filament, which is locally inflated. This thread with a width of ~1.6" (FWHM) is ~6 pc long at the distance of the GC and has a spectrum that can be characterized by a power law or an optically-thin thermal plasma with temperature ~3 keV. The X-ray-emitting material is likely confined within a strand of magnetic field with its strength > 1 mG, not unusual in such radio filaments. These morphological and spectral properties of the radio/X-ray association suggest that magnetic field re-connection is the energy source. Such re-connection events are probably common when flux tubes of antiparallel magnetic fields collide and/or become twisted in and around the diffuse X-ray plumes, representing blowout superbubbles driven by young massive stellar clusters in the GC. The understanding of the process, theoretically predicted in analog to solar flares, can have strong implications for the study of interstellar hot plasma heating, cosmic-ray acceleration and turbulence.
