发表机构
Aix-Marseille Université; CNES; Institut Origines; LAM; Laboratory of Atmospheric and Planetary Physics, STAR Institute, University of Liège; Institut de Recherche en Astrophysique et Planétologie (IRAP); CNES-CNRS-Université de Toulouse; Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-SUPAERO); NASA Langley Research Center; Johns Hopkins University Applied Physics Laboratory; Northumbria University; Weihai Institute for Interdisciplinary Research, Shandong University（艾克斯-马赛大学; 法国国家空间研究中心; 起源研究所; 宇宙学与天体物理学实验室; 列日大学STAR研究所大气与行星物理实验室; 天体物理学与行星学研究所在; 图卢兹大学CNES-CNRS联合机构; 高等航空航天学院; 美国国家航空航天局兰利研究中心; 约翰斯·霍普金斯大学应用物理实验室; 诺森比亚大学; 山东大学威海跨学科研究院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究基于Juno/JEDI数据统计比较木星极光区质子与电子沉降，发现质子能量通量远低于电子，贡献小于2%，但为未来任务提供关键观测目标。
AI 中文摘要
高能电子主导了沉降到木星极光区域的能量，但质子沿同一磁场线沉降，其贡献仍缺乏约束。我们统计比较了木星两个极光子区域——极区（PE）和主发射区（ME）——中质子和电子的沉降能量通量。我们使用了Juno/JEDI从PJ3到PJ66的数据。航天器的磁足点由JRM33和CON2020磁场模型计算，并归属于两个子区域之一，每种粒子的沉降能量通量通过对损失锥内的平均微分强度进行积分获得。在两个子区域中，质子能量通量的中位数比电子低52至223倍，总沉降质子功率小于电子功率的2%。质子通量在子区域中广泛分布，ME中的值高于PE。质子在木星极光能量预算中扮演次要角色，每个子区域在紫外波段辐射估计为5至9吉瓦，有待专门的质子输运建模。它们在莱曼-α线红翼中的多普勒特征，未被HST探测到且难以通过Juno/UVS获取，是即将到来的Juice和Europa Clipper任务的关键观测目标。
英文摘要
Energetic electrons dominate the energy precipitated into Jupiter's auroral regions, but protons precipitate along the same field lines, with a contribution that remains poorly constrained. We statistically compare the precipitating energy flux of protons and electrons in two of Jupiter's auroral sub-regions, the polar (PE) and main (ME) emission regions. We use Juno/JEDI data from PJ3 to PJ66. The magnetic footprint of the spacecraft, computed with the JRM33 and CON2020 field models, is assigned to one of the two sub-regions, and the precipitating energy flux of each species is obtained by integrating over the loss cone the mean differential intensity measured within it. In both sub-regions, the median proton energy flux is 52 to 223 times lower than that of the electrons, and the total precipitated proton power is less than 2% of the electron power. Proton fluxes are broadly distributed across the sub-regions, with higher values in the ME than in the PE. Protons play a secondary role in Jupiter's auroral energy budget, radiating an estimated 5 to 9 GW in the UV per sub-region, pending a dedicated proton transport modelling. Their Doppler signature in the red wing of the Lyman-$α$ line, undetected by HST and difficult to access with Juno/UVS, is a key observable for the upcoming Juice and Europa Clipper missions.
Comments6 pages, 2 figures, submitted to Astronomy & Astrophysics
