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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Observations of magnetospheric ULF waves in connection with the Kelvin-Helmholtz instability at Mercury
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Observations of magnetospheric ULF waves in connection with the Kelvin-Helmholtz instability at Mercury

机译：观察磁性层的ULF波与Kelvin-Helmholtz不稳定在汞

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摘要

The magnetic field data from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft is investigated to establish the presence of magnetospheric ultralow frequency (ULF) waves in connection with 131 previously observed nonlinear Kelvin-Helmholtz (KH) waves at Mercury. Distinct ULF wave signatures are detected in 44 out of the 131 magnetospheric traversals prior to or after observing the KH waves. Of these ULF events, 39 out of 44 are highly coherent at the frequency of maximum power spectral density and occur more often on the dayside magnetosphere than away from it. The waves observed at the dayside magnetosphere, which appear mainly at the duskside and naturally following the KH wave occurrence asymmetry, are significantly different from the eveningside or morningside events and have the following distinct wave characteristics: a polarization mainly in the perpendicular (azimuthal) direction to the mean magnetic field, a wave normal angle closer to the parallel than the perpendicular direction, an absolute ellipticity increasing away from noon, almost exclusively a right-hand polarization, and frequencies in the narrow range of 0.02–0.04 Hz (well below the local Na~+ gyrofrequency and in the same range as the KH waves). The results strongly suggest that the large majority of the ULF waves at the dayside observed in this study are driven by KH waves at the magnetopause and that they occur in the vicinity of a field line resonance, which in turn manifests the importance of the Kelvin-Helmholtz instability in terms of energy and momentum transport throughout Mercury’s magnetosphere.
机译：从水星表面的磁场数据,空间环境,地球化学和测距(MESSENGER)宇宙飞船了建立磁层超低的存在在131年与频率(ULF)波以前观察到非线性Kelvin-Helmholtz(KH)波在汞。在131年44的签名被检测到磁性层的遍历之前或之后观察KH波。从44的频率是高度一致的最大的功率谱密度和更多的发生通常比远离的光面上磁气圈它。磁气圈,主要出现在duskside KH波后和自然出现不对称,是明显不同的从eveningside或晨边高地和事件波具有以下明显的特征:一个主要在垂直极化(方位)方向的磁场,一波法角度接近平行垂直方向,绝对离中午椭圆率增加,几乎只右手极化,在狭窄的频率范围0.02 - -0.04赫兹(远低于当地Na ~ +旋转频率和相同的范围KH波)。强烈建议的大部分ULF波在这项研究中观察到的光面是由磁层和KH波吗他们出现在附近的一个字段共振,进而体现出重要性的Kelvin-Helmholtz不稳定的能量和动量传输水星的磁场。

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