Auroral emissions are a reflection of magnetospheric processes, and, at Jupiter, it is not entirely certain how the morphology of the UV main emission (ME) varies with magnetospheric compression or the strength of the central current sheet. This work leverages the observations from Juno-UVS to link ME variability with magnetospheric states. Novel arc-detection techniques are used to determine new reference ovals for the ME from perijoves 1 through 54, in both hemispheres, and analyse how the size and shape of the ME vary compared to this reference oval. The morphology and brightness of the ME vary in local time: the dawn-side ME is typically expanded and the dusk-side ME typically contracted compared to the reference oval, and the dusk-side ME being typically twice as bright as the dawn-side ME. Both the northern and southern ME, and the day-side and night-side ME, expand and contract from their reference ovals synchronously, which indicates that the variable size of the ME is caused by a process occurring throughout the jovian magnetosphere. The poleward latitudinal shift of the auroral footprint of Ganymede correlates with the poleward motion of the ME, whereas a similar relation is not present for the footprint of Io. Additionally, the expansion of the ME correlates well with an increase in magnetodisc current. These two results suggest that a changing current-sheet magnetic field is partially responsible for the variable size of the ME. Finally, magnetospheric compression is linked to a global ME contraction and brightening, though this brightening occurs predominantly in the day-side ME. This observation, and the observation that the dusk-side ME is typically brighter than the dawn-side ME, stands in contrast to the modelled and observed behaviour of field-aligned currents and thus weakens the theoretical link between field-aligned currents and the generation of the auroral ME.
Enhanced C$_2$H$_2$ absorption within Jupiter's southern auroral oval from Juno UVS observations
朱诺号航天器上的紫外线分光仪反射的太阳光观测被用来研究木星南极乙炔（C $_2$ H $_2$）的分布。我们发现，C $_2$ H $_2$吸收特征的形状在整个极地地区变化显著，这可以用来推断C $_2$ H $_2$丰度的空间变异性。有一个局部区域的增强C $_2$ H $_2$的吸收，这与木星的南极极光的位置相吻合; C $_2$ H $_2$丰度极向极光椭圆是一个因素3高于相邻的静止，非极光极光。这是建立在以前的红外研究，发现增强的C $_2$ H $_2$丰富的北部极光椭圆。这表明木星的高层大气化学受到带电极光粒子流入的强烈影响，并表明有必要开发木星极地区域的离子中性光化学模型。
Meridional variations of C$_2$H$_2$ in Jupiter's stratosphere from Juno UVS observations
朱诺号上的紫外线观测仪记录了从木星反射的远紫外线。这些光谱对高层大气中化学物种的丰度和平流层霾层的分布很敏感。我们结合从第一个30 perijoves的任务，以研究乙炔（C $_2$ H $_2$）在木星平流层的纬向分布的意见。我们发现C $_2$ H $_2$的丰度向两极减少2-4倍，与以前的中红外光谱分析一致。这一结果是从日照率预期的：在赤道附近，紫外线太阳通量较高，允许CH $_4$的紫外线光解产生更多的C $_2$ H $_2$。丰度向两极的减少表明，水平混合率不够快，均匀的纬度分布。
Spatial variability of CH4 and C2H2 absorptions in Jupiter's auroral regions from Juno-UVS observations
University of Liège（列日大学）；Aix-Marseille Université（艾克斯-马赛大学）；National Institute for Astrophysics (INAF-IAPS)（意大利国家天体物理研究所）；Southwest Research Institute（西南研究院）
Energy distributions of precipitating electrons in Jupiter's auroral regions from combined Juno/JADE and Juno/JEDI measurements
Aix-Marseille Université, CNRS, CNES, Institut Origines, LAM（艾克斯-马赛大学，法国国家科学研究中心，法国国家空间研究中心，起源研究所，天体物理学与行星学实验室）；Laboratory of Planetary and Atmospheric Physics, STAR Institute, University of Liège（列日大学，STAR研究所，行星与大气物理实验室）；Université de Toulouse, CNRS, CNES, Institut de Recherche en Astrophysique et Planétologie（图卢兹大学，法国国家科学研究中心，法国国家空间研究中心，天体物理学与行星学研究所以）；Institut Supérieur de l’Aéronautique et de l’Espace (ISAE SUPAERO), Université de Toulouse（图卢兹大学，航空航天高级学院）；Weihai Institute for Interdisciplinary Research, Shandong University（山东大学，威海交叉科学研究院）；Johns Hopkins University Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；Space Science and Engineering Division, Southwest Research Institute（西南研究院，空间科学与工程部）
The precipitation of protons and electrons in Jupiter's auroral regions: a statistical comparison based on Juno/JEDI data
Aix-Marseille Université（艾克斯-马赛大学）；CNES（法国国家空间研究中心）；Institut Origines（起源研究所）；LAM（宇宙学与天体物理学实验室）；Laboratory of Atmospheric and Planetary Physics, STAR Institute, University of Liège（列日大学STAR研究所大气与行星物理实验室）；Institut de Recherche en Astrophysique et Planétologie (IRAP)（天体物理学与行星学研究所在）；CNES-CNRS-Université de Toulouse（图卢兹大学CNES-CNRS联合机构）；Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-SUPAERO)（高等航空航天学院）；NASA Langley Research Center（美国国家航空航天局兰利研究中心）；Johns Hopkins University Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；Northumbria University（诺森比亚大学）；Weihai Institute for Interdisciplinary Research, Shandong University（山东大学威海跨学科研究院）
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）
New Constraints on the Jovian Narrowband Radio Components from Juno/Waves Observations and 3D Geometrical Simulations
Observatoire de Paris, CNRS, PSL, Sorbonne Université, Université Paris Cité（巴黎天文台，法国国家科学研究中心，巴黎文理研究大学，索邦大学，巴黎西岱大学）；Institute of Atmospheric Physics, Czech Academy of Science（捷克科学院大气物理研究所）
Revealing a Systematic High-latitude Current Sheet at Jupiter
Southern University of Science and Technology (SUSTech)（南方科技大学）；the University of Hong Kong（香港大学）；Southwest Research Institute（西南研究院）；University of Texas at San Antonio（德克萨斯大学圣安东尼奥分校）；Beihang University（北京航空航天大学）；Peking University（北京大学）；Mullard Space Science Laboratory, University College London（伦敦大学学院穆拉德空间科学实验室）
