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首页> 外文期刊>Journal of Geophysical Research. Biogeosciences >Hubble Space Telescope imaging of Jupiter's UV aurora during the Galileo orbiter mission
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Hubble Space Telescope imaging of Jupiter's UV aurora during the Galileo orbiter mission

机译：哈勃太空望远镜在伽利略轨道飞行器任务期间对木星紫外线极光的成像

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Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC 2) images of Jupiter's aurora have been obtained close in time with Galileo ultraviolet spectrometer (UVS) spectra and in situ particles, fields, and plasma wave measurements between June 1996 and July 1997, overlapping Galileo orbits G1, G2, G7, G8, and C9. This paper presents HST images of Jupiter's aurora as a first step toward a comparative analysis of the auroral images with the in situ Galileo data. The WFPC 2 images appear similar to earlier auroral images, with the main ovals at similar locations to those observed over the preceding 2 years, and rapidly variable emissions poleward of the main ovals. Further examples have been observed of the equatorward surge of the auroral oval over 140-180 degrees longitude as this region moves from local morning to afternoon. Comparison of the WFPC 2 reference auroral ovals north and south with the VIP4 planetary magnetic field model suggests that the main ovals map along magnetic field lines exceeding 15R(J), and that the Io footprint locations have lead angles of 0-10 degrees from the instantaneous magnetic projection. There was an apparent dawn auroral storm on June 23, 1996, and projections of the three dawn storms imaged with HST to date demonstrate that these appear consistently along the WFPC 2 reference oval. Auroral emissions have been consistently observed from Io's magnetic footprints on Jupiter. Possible systematic variations in brightness are explored, within factor of 6 variations in brightness with time. Images are also presented marked with expected locations of any auroral footprints associated with the satellites Europa and Ganymede, with localized emissions observed at some times but not at other times. [References: 45]
机译：利用伽利略紫外光谱仪（UVS）光谱以及1996年6月至7月间的原位粒子，场和等离子波测量，近距离获取了木星极光的哈勃太空望远镜（HST）广域行星相机2（WFPC 2）图像。 1997年，伽利略轨道G1，G2，G7，G8和C9重叠。本文介绍了木星极光的HST图像，这是通过原位伽利略数据对极光图像进行比较分析的第一步。 WFPC 2图像看起来与早期的极光图像相似，主要椭圆形的位置与之前两年中观察到的位置相似，并且发射速率向主要椭圆形方向快速变化。随着该区域从当地早上到下午移动，在140-180度经度上的极光椭圆的赤道向海浪涌动已观察到更多示例。 WFPC 2参考极光椭圆的南北和南极与VIP4行星磁场模型的比较表明，主椭圆沿超过15R（J）的磁力线映射，并且Io足迹位置的前角为0-10度。瞬时磁投影。 1996年6月23日出现了明显的黎明极光风暴，到目前为止，用HST成像的三场黎明风暴的投影表明，它们沿WFPC 2参考椭圆形一致出现。从木卫一的艾奥磁足迹一直观察到极光发射。探索亮度可能的系统变化，亮度随时间变化6倍。还显示了标有与欧罗巴和木卫三卫星相关的任何极光足迹的预期位置的图像，在某些时间观察到局部发射，但在其他时间观察不到。 [参考：45]

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