论文标题
MHD分解解释了Cygnus x中的散射$γ$ ray发射
MHD decomposition explains diffuse $γ$-ray emission in Cygnus X
论文作者
论文摘要
宇宙射线（CR）扩散是这种带电颗粒与磁波动相互作用的结果。这些波动源自大规模的湍流向较小的空间尺度层叠，分解为三种不同的模式，如$磁铁 - 摩德 - 摩德 - 动力学$（MHD）理论所描述。结果，粒子扩散的描述在很大程度上取决于描述注入湍流的模型。此外，分配给三种模式中每一种的能量量通常不平等，这意味着扩散属性可能从一个区域到另一个区域都不同。在这里，由于检测Cygnus-X恒星形成区域内不同MHD模式的动机，我们研究了一个由两个区域模型中的两个突出来源注射的Crs的3D传输，该模型代表了模式的分布。然后，通过将传播的CR分布与中性气体相卷，我们可以解释该地区的$γ$ -Ray弥漫性发射，这是Fermi-LAT和HAWC协作观察到的。这样的结果代表了将CR可观察物与粒子传输的微型物理连接起来的长期存在的重要步骤。
Cosmic-ray (CR) diffusion is the result of the interaction of such charged particles against magnetic fluctuations. These fluctuations originate from large-scale turbulence cascading towards smaller spatial scales, decomposed into three different modes, as described by $magneto-hydro-dynamics$ (MHD) theory. As a consequence, the description of particle diffusion strongly depends on the model describing the injected turbulence. Moreover, the amount of energy assigned to each of the three modes is in general not equally divided, which implies that diffusion properties might be different from one region to another. Here, motivated by the detection of different MHD modes inside the Cygnus-X star-forming region, we study the 3D transport of CRs injected by two prominent sources within a two-zone model that represents the distribution of the modes. Then, by convolving the propagated CR-distribution with the neutral gas, we are able to explain the $γ$-ray diffuse emission in the region, observed by the Fermi-LAT and HAWC Collaborations. Such a result represents an important step in the long-standing problem of connecting the CR observables with the micro-physics of particle transport.
