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Kinetic models for the exospheres of Jupiter and Saturn

机译：木星和土星系外层的动力学模型

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The exospheric theory based on the Kappa velocity distribution function (VDF) is used to model the exosphere of the giant planets Jupiter and Saturn. Such Kappa velocity distribution functions with an enhanced population of suprathermal particles are indeed often observed in space plasmas and in the space environment of the planets. The suprathermal particles have significant effects on the escape flux, density and temperature profiles of the particles in the exosphere of the giant planets. The polar wind flux becomes several orders larger when suprathermal electrons are considered, so that the planetary ionosphere becomes then a significant source for their inner magnetosphere. Moreover, the number density of the particles decreases slower as a function of the altitude when a Kappa distribution is considered instead of a Maxwellian one. Two-dimensional maps of density are calculated for typical values of the temperatures. The exospheric formalism is also applied to study the escape flux from the exospheres of Io and Titan, respectively, moons of Jupiter and Saturn.
机译：基于Kappa速度分布函数（VDF）的系外层理论用于对木星和土星等巨型行星的系外层建模。实际上，经常在空间等离子体和行星的空间环境中观察到这种具有超热粒子增加的Kappa速度分布函数。超热粒子对巨型行星系外层中粒子的逸散通量，密度和温度分布具有重要影响。当考虑超热电子时，极风通量会增大几个数量级，因此行星电离层便成为其内部磁层的重要来源。此外，当考虑用卡伯分布代替麦克斯韦分布时，随着高度的增加，颗粒数密度的降低速度会变慢。计算出典型温度值的二维密度图。大气外形式主义也被用于研究分别来自木卫六和土星卫星伊奥和泰坦的大气圈的逃逸通量。

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