The Atmospheric Radiation Interaction Simulator (AtRIS): Description and Validation
The Atmospheric Radiation Interaction Simulator (AtRIS): Description and Validation
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DOI：
10.1029/2018ja026042
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发表时间：
2019-01
期刊：
影响因子：
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通讯作者：
S. Banjac;K. Herbst;B. Heber
中科院分区：
文献类型：
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作者：
S. Banjac;K. Herbst;B. Heber
我们推出了大气辐射相互作用模拟器 (AtRIS)，这是一种新开发的基于 GEANT4 的代码，专门用于对通过各种（外）行星大气层的辐射传播进行参数化研究。其主要目的是对依赖于高度的大气二次粒子环境进行建模并计算离子对生成速率，这是大气化学模型的强制性输入，以便直接表征所建模行星的可居住性。之前已经开发了类似的代码（例如 PLANETOCOSMICS；Desorgher 等人）；然而，到目前为止，没有人在大气和风化层的规格方面拥有必要的灵活性，而这对于模拟太阳系外的行星来说是必需的。在这里，我们提供了 AtRIS 的详细描述及其针对地球测量的验证。为了验证，我们展示了与地球测量值的比较。因此，重点是大气高度相关的电离、表面μ子、中子通量以及初级质子通量。此外，还显示了基于 AtRIS 和 PLANETOCOSMICS 计算的单能质子能量损失的比较。我们的目标是证明 AtRIS 的有效性及其对未来研究（例如潜在（类地）系外行星）的重要性。
We present the Atmospheric Radiation Interaction Simulator (AtRIS), a newly developed GEANT4‐based code tailored specifically to enable parametric studies of radiation propagation through various (exo)planetary atmospheres. Its main purpose is to model the altitude‐dependent atmospheric secondary particle environment and to calculate the ion pair production rates, which are a mandatory input for atmospheric chemistry models in order to, for example, directly characterize the habitability of the modeled planet. Similar codes have been developed previously (e.g., PLANETOCOSMICS; Desorgher, et al., ); however, until now, none possesses the necessary flexibility in the specification of the atmosphere and the regolith that is necessary to model planets outside our solar system. Here we provide a detailed description of AtRIS and its validation against earthbound measurements. For validation, we show comparisons against Earth measurements. Thereby, the focus is on the atmospheric altitude‐dependent ionization, the surface muon, and the neutron fluxes, as well as the primary proton fluxes. Furthermore, a comparison of the computed energy losses of monoenergetic protons based on AtRIS and PLANETOCOSMICS is shown. Our aim is to demonstrate the validity of AtRIS and its importance for future studies on, for example, potential (Earth‐like) exoplanets.