On the Origin of Observed Cosmic-Ray Spectrum Below 100 TV
On the Origin of Observed Cosmic-Ray Spectrum Below 100 TV
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DOI：
10.3847/1538-4357/ac7049
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发表时间：
2021-05
期刊：
影响因子：
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通讯作者：
M. Malkov;I. Moskalenko
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文献类型：
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作者：
M. Malkov;I. Moskalenko
最近对太伏特刚性域中的主要和次要宇宙射线（CR）物种的精确测量揭示了它们的光谱在0.5和50 TV之间的凹凸。我们认为，局部冲击可以通过将先前存在的低于50 TV的CRs的刚度增加约1.5倍来产生这样的颠簸。低于~ 0.5 TV的再加速粒子与星际介质流发生了对流，无法到达太阳，因此产生了碰撞。这一单一的普遍过程是导致在100 TV以下刚性范围内观察到的所有CR物种光谱的原因。我们提出一个可行的激波候选者是距离太阳3.2 pc的Epsilon Eridani恒星，它与当地磁场的方向很好地对齐。其他的冲击，比如古老的超新星壳，可能会产生类似的效果。我们提供了一个简单的公式，公式(9)，它再现了所有CR物质的光谱，只有两个不可调的激波参数，唯一地从质子数据中导出。我们展示了我们的形式如何预测氦和碳光谱以及B/C比。
Recent precise measurements of primary and secondary cosmic-ray (CR) species in the teravolt rigidity domain have unveiled a bump in their spectra, located between 0.5 and 50 TV. We argue that a local shock may generate such a bump by increasing the rigidity of the preexisting CRs below 50 TV by a mere factor of ∼1.5. Reaccelerated particles below ∼0.5 TV are convected with the interstellar medium flow and do not reach the Sun, thus creating the bump. This single universal process is responsible for the observed spectra of all CR species in the rigidity range below 100 TV. We propose that one viable shock candidate is the Epsilon Eridani star at 3.2 pc from the Sun, which is well aligned with the direction of the local magnetic field. Other shocks, such as old supernova shells, may produce a similar effect. We provide a simple formula, Equation (9), that reproduces the spectra of all CR species with only two nonadjustable shock parameters, uniquely derived from the proton data. We show how our formalism predicts helium and carbon spectra and the B/C ratio.