: the driver of giant planet atmospheres
: the driver of giant planet atmospheres
复制标题
：巨大行星大气层的驱动力
DOI：
--
复制
发表时间：
2006
期刊：
影响因子：
--
通讯作者：
A. Aylward
中科院分区：
文献类型：
--
作者：
S. Miller;T. Stallard;Chris Smith;G. Millward;H. Melin;M. Lystrup;A. Aylward
本文综述了近年来利用分子离子探测巨行星上层大气的物理和化学研究进展。这种离子被证明是一个很好的示踪剂的能量输入到木星（J），土星（S）和天王星（U）。它还作为一个“恒温器”，抵消由于粒子沉淀通过冷却到空间（J和U）而增加的能量输入。计算机模型已经确定，这也是电离层传导性的主要因素。极光极区电场和磁场的耦合导致离子风，离子风反过来又驱动中性环流系统（J和S）。这后两种效应，依赖于，也导致非常大的加热项，土星约为5×1012 W，木星大于1014 W，行星范围;这些项与土星约2.5×1011 W的太阳极端紫外线吸收和木星1012 W的太阳极端紫外线吸收相比。 因此，在解释为什么巨行星大气层顶部的温度要比太阳输入单独解释的温度高得多（数百开尔文）方面，它发挥了重要作用。
We present a review of recent developments in the use of molecular ion as a probe of physics and chemistry of the upper atmospheres of giant planets. This ion is shown to be a good tracer of energy inputs into Jupiter (J), Saturn (S) and Uranus (U). It also acts as a ‘thermostat’, offsetting increases in the energy inputs owing to particle precipitation via cooling to space (J and U). Computer models have established that is also the main contributor to ionospheric conductivity. The coupling of electric and magnetic fields in the auroral polar regions leads to ion winds, which, in turn, drive neutral circulation systems (J and S). These latter two effects, dependent on , also result in very large heating terms, approximately 5×1012 W for Saturn and greater than 1014 W for Jupiter, planet-wide; these terms compare with approximately 2.5×1011 W of solar extreme UV absorbed at Saturn and 1012 W at Jupiter. Thus, is shown to play a major role in explaining why the temperatures of the giant planets are much greater (by hundreds of kelvin) at the top of the atmosphere than solar inputs alone can account for.
影响因子：
56.9
作者：
BERARDI, AC;WANG, AL;SCADDEN, DT
通讯作者：
SCADDEN, DT