Jupiter's Aurora Observed With HST During Juno Orbits 3 to 7
Jupiter's Aurora Observed With HST During Juno Orbits 3 to 7
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DOI：
10.1002/2017ja025046
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发表时间：
2018-05
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通讯作者：
D. Grodent;B. Bonfond;Z. Yao;J. Gérard;A. Radioti;M. Dumont;B. Palmaerts;A. Adriani;S. Badman;E. Bunce;J. Clarke;J. Connerney;G. Gladstone;T. Greathouse;T. Kimura;W. Kurth;B. Mauk;D. McComas;J. Nichols;G. Orton;L. Roth;J. Saur;P. Valek
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作者：
D. Grodent;B. Bonfond;Z. Yao;J. Gérard;A. Radioti;M. Dumont;B. Palmaerts;A. Adriani;S. Badman;E. Bunce;J. Clarke;J. Connerney;G. Gladstone;T. Greathouse;T. Kimura;W. Kurth;B. Mauk;D. McComas;J. Nichols;G. Orton;L. Roth;J. Saur;P. Valek
在2016年11月30日至2017年7月18日的8个月期间，哈勃太空望远镜与NASA-朱诺使命同时收集了大量木星紫外极光的观测结果。这些哈勃观测涵盖了朱诺轨道3至7，在此期间，朱诺原位和遥感仪器以及其他观测站获得了关于木星磁层及其与极光电离层联系的大量前所未有的信息。众所周知，木星的紫外极光变化迅速，时间尺度从几秒到一个木星旋转。本研究的主要目的是提供全球紫外极光形态的简化描述，可用于与其他数量，如朱诺号获得的数量进行比较。这代表了一种全新的方法，可以从中推断出不同形态之间的逻辑联系。为此，我们定义了三个极光分区，在其中我们评估极光发射功率作为时间的函数。同时，我们定义了六个极光形态的家庭，使我们能够量化的极光发射的空间分布的变化。这些变化与木星磁层状态的变化有关，可能受到木卫一和木卫一等离子体环以及上游行星际介质中的条件的影响。研究表明，在木星近木星时刻（PJ 03 ~ PJ 07）前后的5 ~2周时间内，极光形态的演变是不同的，表明在这5 ~2周时间内，木星磁层呈现出不同的状态。
A large set of observations of Jupiter's ultraviolet aurora was collected with the Hubble Space Telescope concurrently with the NASA‐Juno mission, during an eight‐month period, from 30 November 2016 to 18 July 2017. These Hubble observations cover Juno orbits 3 to 7 during which Juno in situ and remote sensing instruments, as well as other observatories, obtained a wealth of unprecedented information on Jupiter's magnetosphere and the connection with its auroral ionosphere. Jupiter's ultraviolet aurora is known to vary rapidly, with timescales ranging from seconds to one Jovian rotation. The main objective of the present study is to provide a simplified description of the global ultraviolet auroral morphology that can be used for comparison with other quantities, such as those obtained with Juno. This represents an entirely new approach from which logical connections between different morphologies may be inferred. For that purpose, we define three auroral subregions in which we evaluate the auroral emitted power as a function of time. In parallel, we define six auroral morphology families that allow us to quantify the variations of the spatial distribution of the auroral emission. These variations are associated with changes in the state of the Jovian magnetosphere, possibly influenced by Io and the Io plasma torus and by the conditions prevailing in the upstream interplanetary medium. This study shows that the auroral morphology evolved differently during the five ~2 week periods bracketing the times of Juno perijove (PJ03 to PJ07), suggesting that during these periods, the Jovian magnetosphere adopted various states.