Fluid models capturing Farley–Buneman instabilities

IF 1.7 4区 地球科学 Q3 ASTRONOMY & ASTROPHYSICS Annales Geophysicae Pub Date : 2023-07-13 DOI:10.5194/angeo-41-281-2023
E. Rojas, K. Burns, D. Hysell
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Abstract

Abstract. It is generally accepted that modeling Farley–Buneman instabilities requires resolving ion Landau damping to reproduce experimentally observed features. Particle-in-cell (PIC) simulations have been able to reproduce most of these but at a computational cost that severely affects their scalability. This limitation hinders the study of non-local phenomena that require three dimensions or coupling with larger-scale processes. We argue that a form of the five-moment fluid system can recreate several qualitative aspects of Farley–Buneman dynamics such as density and phase speed saturation, wave turning, and heating. Unexpectedly, these features are still reproduced even without using artificial viscosity to capture Landau damping. Comparing the proposed fluid models and a PIC implementation shows good qualitative agreement.
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捕捉法利-布曼不稳定性的流体模型
摘要人们普遍认为,法利-布曼不稳定性的建模需要解析离子朗道阻尼来重现实验观察到的特征。细胞内粒子(PIC)模拟已经能够重现其中的大部分,但其计算成本严重影响了其可扩展性。这一限制阻碍了需要三维或与更大规模过程耦合的非局部现象的研究。我们认为,五矩流体系统的一种形式可以重现法利-布曼动力学的几个定性方面,如密度和相速度饱和、波浪转向和加热。出乎意料的是,即使没有使用人工粘度来捕获朗道阻尼,这些特征仍然可以再现。将所提出的流体模型与PIC实现进行比较,结果显示出良好的定性一致性。
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来源期刊
Annales Geophysicae
Annales Geophysicae 地学-地球科学综合
CiteScore
4.30
自引率
0.00%
发文量
42
审稿时长
2 months
期刊介绍: Annales Geophysicae (ANGEO) is a not-for-profit international multi- and inter-disciplinary scientific open-access journal in the field of solar–terrestrial and planetary sciences. ANGEO publishes original articles and short communications (letters) on research of the Sun–Earth system, including the science of space weather, solar–terrestrial plasma physics, the Earth''s ionosphere and atmosphere, the magnetosphere, and the study of planets and planetary systems, the interaction between the different spheres of a planet, and the interaction across the planetary system. Topics range from space weathering, planetary magnetic field, and planetary interior and surface dynamics to the formation and evolution of planetary systems.
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