The Jovian magnetosphere is complicated by the multiple plasma sources and ion species present within it, as well as fast rotation with its dipole axis titled from its rotational axis. To date global models of Jovian have neglected the presence of the different ion species as well as the tilted nature of the dipole axis. This paper reports the results of the first multi-fluid global modeling of these effects in a single self-consistent study for processes occurring in the outer magnetosphere. In the inner magnetosphere the model densities are shown to be comparable to observed densities with much of the density variables due to the wobble. The wobble enables plasma to be transported to higher latitudes and then centrifugal acceleration leads to radial transport of the plasma. At the interface between the middle and outer magnetosphere, the wobble produces a sinusoidal modulation of the plasma properties, which yields at a fixed observing point two density peaks, each with the planetary period. However, because of solar wind forcing and the fast rotation of Jupiter, torques are exerted on the outer magnetospheric plasma such that the azimuthal speed between the southern and northern hemispheres are unequal. This leads to the asymmetric square wave modulation of the plasma properties in the outer magnetosphere such that only one density peak is seen each planetary period in the outer magnetosphere. This differential speed leads to reconnection in the tail at the planetary period and enhanced ejection of plasma down the tail at the planetary period. These processes could explain the periodicity seen in the New Horizons' data without the need for invoking arbitrary solar wind conditions. The energetic particles generated by these processes are shown to map to the arc-like structures seen in the dusk side auroral features.
The large-scale energetic ion layer in the high latitude Jovian magnetosphere as revealed by Ulysses/HI-SCALE cross-field intensity-gradient measurements
在先驱者11号任务之后，NASA第二次对高纬度木星磁层进行了调查，并为我们提供了研究磁盘上方巨磁层结构和动力学的机会。Kivelson（1976）和Kennel & Coroniti（1979）报告说，先驱者11号在高纬度地区观测到的高能粒子强度与在等离子体片中测量到的强度处于同一水平，并推断它们与磁盘模型不一致。天文学家的观测支持了在木星外高纬度磁层中存在大规模高能离子和电子层的观点（Cowley et al.1996; Anagnostopoulos et al. 2001）。本研究通过研究适当的交叉B场各向异性，以监测离子向北/向南的强度梯度，对高纬木星外磁层中大尺度高能离子层的存在进行了一些进一步的测试。特别是，我们检查了具有大回转半径（0.5-1.6MeV质子和>2.5MeV重（Z>5）离子）的高能离子的Ulysses/HI-SCALE观测，以便将瞬时强度变化与遥感强度梯度进行比较。我们的分析证实了高能粒子层的存在，在北半球，在入境轨道的飞行器在中纬度地区，在南高纬度的黄昏侧磁层，在航天器轨迹的出站段。我们的ESTA/HI-SCALE数据分析还提供了证据，探测到一个充满活力的质子磁层顶边界层在航天器的出站轨迹。在木星近距离飞越期间，几乎永久性地出现了南北交替的强度梯度，这表明高纬度层似乎是高能粒子的第三个主要区域，与辐射带和磁盘共存。
Revealing the Spatial Distribution of Dust and Plasma Solitary Waves in Jupiter's Innermost Magnetosphere Using Juno Waves Observations
UCLA Department of Earth, Planetary, and Space Sciences（加州大学洛杉矶分校地球、行星与空间科学系）；UCLA SPACE Institute（加州大学洛杉矶分校SPACE研究所）；University of Iowa, Department of Physics and Astronomy（爱荷华大学物理与天文学系）；Princeton University, Department of Astrophysical Sciences（普林斯顿大学天体物理学系）；Jet Propulsion Laboratory（喷气推进实验室）；Southwest Research Institute（西南研究院）
Generation mechanism and beaming of Jovian nKOM from 3D numerical modeling of Juno/Waves observations
LESIA, Observatoire de Paris, CNRS, PSL, Sorbonne Université, Université Paris Cité（巴黎天文台）；National Institute of Technology (KOSEN), Niihama College（国立技术学院新居滨高专）；Observatoire Radioastronomique de Nançay, ORN, Observatoire de Paris, CNRS, PSL, Université d’Orléans（南希射电天文台）；School of Cosmic Physics, DIAS Dunsink Observatory, Dublin Institute for Advanced Studies（都柏林高等研究院邓辛克天文台宇宙物理学院）
