Abstract High energy cosmic rays reach the surface of the Sun and start showers with thousands of secondary particles. Most of them will be absorbed by the Sun, but a fraction of the neutral ones will escape and reach the Earth. Here we incorporate a new ingredient that is essential to understand the flux of these solar particles: the cosmic ray shadow of the Sun. We use Liouville’s theorem to argue that the only effect of the solar magnetic field on the isotropic cosmic ray flux is to interrupt some of the trajectories that were aiming to the Earth and create a shadow. This shadow reveals the average solar depth crossed by cosmic rays of a given rigidity. The absorbed cosmic ray flux is then processed in the thin Solar surface and, assuming that the emission of neutral particles by low-energy charged particles is isotropic, we obtain (i)a flux of gammas that is consistent with Fermi-LAT observations, (ii) a flux of 100–300 neutrons/(year m2) produced basically in the spallation of primary He nuclei, and (iii) a neutrino flux that is above the atmospheric neutrino background at energies above 0.1–0.6 TeV (depending on the solar phase and the zenith inclination). More precise measurements of the cosmic ray shadow and of the solar gamma flux, together with the possible discovery of the neutron and neutrino signals, would provide valuable information about the magnetic field, the cycle, and the interior of the Sun.

中文翻译：

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TeV能量下的太阳：伽马、中子、中微子和宇宙射线阴影

摘要 高能宇宙射线到达太阳表面并以数千个次级粒子开始阵雨。它们中的大部分会被太阳吸收，但一小部分中性的会逃逸并到达地球。在这里，我们加入了一种对理解这些太阳粒子的通量至关重要的新成分：太阳的宇宙射线阴影。我们使用刘维尔定理论证太阳磁场对各向同性宇宙射线通量的唯一影响是中断一些瞄准地球的轨迹并产生阴影。这个阴影揭示了给定刚度的宇宙射线穿过的平均太阳深度。吸收的宇宙射线通量然后在薄的太阳表面进行处理，假设低能带电粒子发射的中性粒子是各向同性的，我们获得了 (i) 与 Fermi-LAT 观测一致的伽马通量，(ii) 100-300 中子/（年 m2）的通量，基本上是在初级 He 核的散裂中产生的，以及 (iii) 中微子通量高于大气中微子背景，能量高于 0.1-0.6 TeV（取决于太阳相位和天顶倾角）。对宇宙射线阴影和太阳伽马通量进行更精确的测量，再加上可能发现的中子和中微子信号，将提供有关太阳磁场、周期和内部的宝贵信息。6 TeV（取决于太阳相位和天顶倾角）。对宇宙射线阴影和太阳伽马通量进行更精确的测量，再加上可能发现的中子和中微子信号，将提供有关太阳磁场、周期和内部的宝贵信息。6 TeV（取决于太阳相位和天顶倾角）。对宇宙射线阴影和太阳伽马通量进行更精确的测量，再加上可能发现的中子和中微子信号，将提供有关太阳磁场、周期和内部的宝贵信息。