Enhanced transport in the polar mesosphere of Jupiter: Evidence from Cassini UVIS helium 584 Å airglow
Enhanced transport in the polar mesosphere of Jupiter: Evidence from Cassini UVIS helium 584 Å airglow
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木星极地中间层的运输增强：卡西尼号 UVIS 氦气 584 Å 气辉的证据
DOI：
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
J. Ajello
中科院分区：
文献类型：
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作者：
C. Parkinson;A. Stewart;A. Wong;Y. Yung;J. Ajello
[1]木星极光区域的涡旋扩散廓线(K)没有得到很好的确定。然而，由于强烈的极光能量输入，涡旋混合预计会更加有效，可能是极地地区重烃生产增加的原因。在这篇文章中，我们通过比较卡西尼号紫外线成像光谱仪(UVIS)在2000年飞越木星时的观测结果和辐射传输计算，估计了木星极光区涡旋混合的增加
[1] The eddy diffusion profile (K) in the auroral regions of Jupiter is not well determined. However, because of the intense auroral energy input, eddy mixing is expected to be much more effective and may be responsible for the enhancement of heavy hydrocarbon production in the polar region. In this paper, we estimate the increased eddy mixing in the Jovian auroral regions by comparing the Cassini Ultraviolet Imaging Spectrograph (UVIS) observations during the 2000 Jupiter flyby with radiative transfer calculations