期刊
JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
卷 121, 期 2, 页码 1273-1293出版社
AMER GEOPHYSICAL UNION
DOI: 10.1002/2015JA021997
关键词
kinetic simulation; Ganymede; Hall MHD; Galileo
资金
- Space Hazards Induced near Earth by Large, Dynamic Storms (SHIELDS) project - U.S. Department of Energy through the Los Alamos National Laboratory Directed Research and Development program [DE-AC52-06NA25396]
- INSPIRE NSF grant [PHY-1513379]
- NASA [NNX15AH28G, NNX15AJ68G]
- NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center
- Yellowstone by NCAR's Computational and Information Systems Laboratory
- National Science Foundation
- NASA [804283, NNX15AJ68G, 807721, NNX15AH28G] Funding Source: Federal RePORTER
We have recently developed a new modeling capability to embed the implicit particle-in-cell (PIC) model iPIC3D into the Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme magnetohydrodynamic (MHD) model. The MHD with embedded PIC domains (MHD-EPIC) algorithm is a two-way coupled kinetic-fluid model. As one of the very first applications of the MHD-EPIC algorithm, we simulate the interaction between Jupiter's magnetospheric plasma and Ganymede's magnetosphere. We compare the MHD-EPIC simulations with pure Hall MHD simulations and compare both model results with Galileo observations to assess the importance of kinetic effects in controlling the configuration and dynamics of Ganymede's magnetosphere. We find that the Hall MHD and MHD-EPIC solutions are qualitatively similar, but there are significant quantitative differences. In particular, the density and pressure inside the magnetosphere show different distributions. For our baseline grid resolution the PIC solution is more dynamic than the Hall MHD simulation and it compares significantly better with the Galileo magnetic measurements than the Hall MHD solution. The power spectra of the observed and simulated magnetic field fluctuations agree extremely well for the MHD-EPIC model. The MHD-EPIC simulation also produced a few flux transfer events (FTEs) that have magnetic signatures very similar to an observed event. The simulation shows that the FTEs often exhibit complex 3-D structures with their orientations changing substantially between the equatorial plane and the Galileo trajectory, which explains the magnetic signatures observed during the magnetopause crossings. The computational cost of the MHD-EPIC simulation was only about 4 times more than that of the Hall MHD simulation. Key Points
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据