Jupiter has a strong magnetic field, and a huge magnetosphere is formed through the solar wind-Jupiter interaction. The generated magnetosphere–ionosphere system is reproduced based on the 9-component Magnetohydrodynamics (MHD) and the current conservation in the ionosphere. Assuming Io plasma emission rate 1.4 t/sec, this paper reproduces self-consistently global magnetic configuration, generations of the field-aligned current (FAC) and aurora, formation of the Io plasma disk at 8–20 R_J, plasma corotation, instability in the plasma disk, transition from the Io plasma disk to the plasma sheet at 20–150 R_J, and the plasmoid ejection. The rotating Io plasma in the disk forms instabilities that promotes radial diffusion. H⁺ is supplied from the ionosphere along high-latitude magnetic field lines and mixed with heavy ions around 15–20 R_J. Beyond 20 R_J, mixed plasma diffuses further outward by the centrifugal force that can exceed magnetic tension. In the ionosphere, the main oval occurs at 13.7°–15.5° colatitude. The Io disk is inner side of magnetic field lines traced from the low-latitude edge of the main oval. Along magnetic field lines, the main oval is mapped from the outer edge of the Io disk to the entire plasma sheet accompanying rotation delay. Due to the corotation limit, convection is accompanied by plasmoid ejection. Back reaction of plasmoid ejection affects even transport process in the Io disk. The downward FAC occurs in the polar cap showing variability. The region of externally driven Dungey convection seems quite narrow.

中文翻译：

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木星磁层的全球模拟：从 Io 等离子体盘到等离子体片的过渡结构

木星有很强的磁场，通过太阳风-木星相互作用形成了巨大的磁层。生成的磁层-电离层系统是根据 9 分量磁流体动力学 (MHD) 和电离层中的电流守恒再现的。假设 Io 等离子体发射率为 1.4 t/sec，本文再现了自洽的全局磁构型、场对齐电流 (FAC) 和极光的产生、8-20 R _J的 Io 等离子体盘的形成、等离子体共转、不稳定性在等离子盘中，从 Io 等离子盘过渡到 20-150 R _J的等离子片，以及等离子团喷射。圆盘中旋转的 Io 等离子体形成不稳定性，促进径向扩散。H ⁺沿着高纬度磁场线从电离层提供，并与大约 15-20 R _{J 的}重离子混合。超过 20 R _J，混合等离子体通过可以超过磁张力的离心力进一步向外扩散。在电离层中，主要的椭圆发生在 13.7°–15.5° 的纬度。Io 盘是从主椭圆的低纬度边缘追踪的磁场线的内侧。沿着磁场线，主椭圆从 Io 盘的外边缘映射到伴随着旋转延迟的整个等离子体片。由于共转限制，对流伴随着等离子体喷射。等离子体喷射的反向反应甚至影响 Io 盘中的传输过程。向下的 FAC 发生在极冠中，显示出变化。外部驱动的 Dungey 对流区域似乎相当狭窄。