论文标题
宇宙射线光谱和偶极性各向异性的三组分模型
A Three-component Model for Cosmic-ray Spectrum and Dipole Anisotropy
论文作者
论文摘要
使用三组分的多尺度扩散模型，我们表明可以使用合理的参数来解释宇宙射线（CR）质子（CR）质子和氦各向异性。该模型包括与超新星残留物（SNR）相关的附近来源，该来源引起了Geminga Pulsar，Geminga Pulsar，一个银河中心的源，以及与银河盘相关的组件。 TEV下方的CR通量由磁盘组件主导。需要大约18 Myr的CRS连续注射的中心源来解释以上100 TEV以上的各向异性。通过所有SNR注入通用CR光谱的假设，附近的来源可以通过在星际磁场上缓慢扩散在地球上观察到地球的TEV光谱凸起，该磁场需要在田间线和视觉线之间的视线和磁性弱的磁性湍流之间的角度约5^{\ circ} $，并具有$ 5^{\ circ} $ m _ {\ text {a}} \大约0.1 $。考虑到该磁场对银河尺度各向异性的调节，在准局部方法中，该场可以针对右升升，约$ -90^{\ circ} $，在备量坐标系统中的偏差约为$ -90^{\ cirp} $。
Using a three-component, multi-scale diffusion model, we show that the cosmic-ray (CR) proton and helium spectra and the dipole anisotropy can be explained with reasonable parameters. The model includes a nearby source associated with the supernova remnant (SNR) that gave rise to the Geminga pulsar, a source at the Galactic center, and a component associated with the Galactic disk. The CR flux below TeV is dominated by the disk component. The center source with a continuous injection of CRs starting about 18 Myr ago is needed to explain the anisotropy above 100 TeV. With the assumption of universal CR spectra injected by all SNRs, the nearby source can produce a TeV spectral bump observed at Earth via slow diffusion across the interstellar magnetic field, which needs to have an angle $ θ\approx 5^{\circ} $ between the field line and the line of sight toward the source, and have weak magnetic turbulence with the Alfvén Mach number $ M_{\text{A}}\approx 0.1 $. Considering the modulation of the Galactic-scale anisotropy by this magnetic field, in a quasi-local approach the field may be directed at a right ascension about $ -90^{\circ} $ and a declination about $ -7.4^{\circ} $ in the equatorial coordinate system.
