论文标题
恒星：康普顿的逆康普顿从宁静的太阳和凯夫到TEV的星星发射
StellarICS: Inverse Compton Emission from the Quiet Sun and Stars from keV to TeV
论文作者
论文摘要
十年前，对伽玛射线中安静的太阳的研究始于十年，并迅速引起了人们的兴趣。来自安静的太阳的伽马射线是由宇宙射线（CRS）与其表面（磁盘分量）及其光子场（空间扩展的逆 - compton组件，IC）产生的。后一个组件最大靠近太阳，即使在大角距离上也延伸到整个天空上，它也在背景上。现在，它首先用白生检测到，现在对其具有高统计学意义的费米 - 拉特研究。 对IC分量的观察使我们能够在太阳活性和极性的各个时期获得有关靠近太阳和地球层的CR电子和正电子的信息。他们允许了解CR相互作用和传播接近恒星，在地球层和太阳表面上，并了解太阳本身，环境和活动。太阳观测的分析通常是模型驱动的。因此，及时且需要及时且需要从精确的CR测量中获得的模型计算和约束的进步。 在这里，我们介绍了恒星代码，以计算来自太阳的伽马射线发射以及单星。该代码公开可用，科学界广泛使用它来分析费米 - 拉特数据。 Fermi-LAT协作已将其用于生产使用FSSC Fermi工具发布的太阳能模型。我们的建模为分析和解释太阳和恒星的高能数据提供了基础。 在介绍了有关各种CR测量结果的Fermi-LAT能量范围内更新的太阳能模型的示例之后，我们将模型扩展到Kev，Mev和TeV Energies，以预测未来可能的望远镜，例如Amego，Gecco，Gecco，E-ASTROGAM，HAWC，HAWC，LHAASO，LHAASO，SWGO，SWGO，SWGO，和现在的X-Ray telescopes。我们还提出了一些最接近和最发光的恒星的预测。
The study of the quiet Sun in gamma rays started over a decade ago, and rapidly gained a wide interest. Gamma rays from the quiet Sun are produced by Cosmic Rays (CRs) interacting with its surface (disk component) and with its photon field (spatially extended inverse-Compton component, IC). The latter component is maximum close to the Sun and it is above the background even at large angular distances, extending over the whole sky. First detected with EGRET, it is studied now with Fermi-LAT with high statistical significance. Observations of the IC component allow us to obtain information on CR electrons and positrons close to the Sun and in the heliosphere for the various periods of solar activity and polarity. They allow to learn about CR interactions and propagation close to stars, in the heliosphere and on the solar surface, and to understand the Sun itself, its environment, and its activity. Analyses of solar observations are usually model-driven. Hence advances in model calculations and constraints from precise CR measurements are timely and needed. Here we present our StellarICS code to compute the gamma-ray IC emission from the Sun and also from single stars. The code is publicly available and it is extensively used by the scientific community to analyze Fermi-LAT data. It has been used by the Fermi-LAT collaboration to produce the solar models released with the FSSC Fermi Tools. Our modeling provides the basis for analyzing and interpreting high-energy data of the Sun and of stars. After presenting examples of updated solar IC models in the Fermi-LAT energy range that account for the various CR measurements, we extend the models to keV, MeV, and TeV energies for predictions for future possible telescopes such as AMEGO, GECCO, e-ASTROGAM, HAWC, LHAASO, SWGO, and present X-ray telescopes. We also present predictions for some of the closest and most luminous stars.
