木星磁盘中的径向输运和等离子体加热
Radial transport and plasma heating in Jupiter's magnetodisc
摘要：
从伽利略偏最小二乘数据导出的木星磁层的离子温度被观察到增加约一个数量级从10到40木星半径。这表明存在抵消膨胀等离子体的绝热冷却效应的热源。已经有不同的尝试来解释这种现象，包括基于通量管扩散的磁流体动力学（MHD）湍流加热模型[Saur，Astrophys. J. Lett.，602，L137，2004]。我们探讨了一种基于平流的交替湍流加热模型，类似于太阳风加热中常用的模型。伽利略磁强计（MAG）数据的频谱分析的基础上，我们发现，所观察到的MHD湍流可能提供所需的加热来解释一些等离子体温度的增加。这表明，平流是一个更合适的方式来描述径向传输的等离子体在木星磁层超过10木星半径。
英文摘要：
The ion temperature of the magnetosphere of Jupiter derived from Galileo PLS data was observed to increase by about an order of magnitude from 10 to 40 Jupiter radii. This suggests the presence of heating sources that counteract the adiabatic cooling effect of expanding plasma. There have been different attempts of explaining this phenomena, including a magnetohydrodynamic (MHD) turbulent heating model which is based on flux tube diffusion [Saur, Astrophys. J. Lett., 602, L137, 2004]. We explore an alternate turbulent heating model based on advection, similar to models commonly used in solar wind heating. Based on spectral analysis of Galileo magnetometer (MAG) data, we find that observed MHD turbulence could potentially provide the required heating to explain some of the increase in plasma temperature. This indicates that advection is a more appropriate way to describe radial transport of plasma in the jovian magnetosphere beyond 10 Jupiter radii.
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