论文标题
宇宙射线光环的形成：主要宇宙射线的银河系光谱
Formation of the cosmic-ray halo: Galactic spectrum of primary cosmic rays
论文作者
论文摘要
在银河系磁盘周围的一维宇宙射线（CR）光环的自洽模型由限制到最小数量的自由参数。已经证明，MHD波的湍流级联反应不一定在光环形成中起着至关重要的作用。取而代之的是，距离磁盘距离的Alfven速度的增加导致了湍流红移的有效通用机制，从而增强了自我生成的MHD波的CR散射。结果，在较低能量下计算出的Cr光环的尺寸取决于光晕鞘，这是圆盘周围的能量依赖区域，cr逃逸纯粹是纯粹的对流。在足够高的能量下，光环大小是由离子气体分布的特征厚度设置的。质子的计算出的银河光谱与观测值显示出显着的一致性，重现了〜0.6 TEV的光谱断裂位置，并且光谱形状最高为〜10 TEV。
A self-consistent model of a one-dimensional cosmic-ray (CR) halo around the Galactic disk is formulated with the restriction to a minimum number of free parameters. It is demonstrated that the turbulent cascade of MHD waves does not necessarily play an essential role in the halo formation. Instead, an increase of the Alfven velocity with distance to the disk leads to an efficient generic mechanism of the turbulent redshift, enhancing CR scattering by the self-generated MHD waves. As a result, the calculated size of the CR halo at lower energies is determined by the halo sheath, an energy-dependent region around the disk beyond which the CR escape becomes purely advective. At sufficiently high energies, the halo size is set by the characteristic thickness of the ionized gas distribution. The calculated Galactic spectrum of protons shows a remarkable agreement with observations, reproducing the position of spectral break at ~ 0.6 TeV and the spectral shape up to ~ 10 TeV.
