Abstract

The subsolar point on Jupiter’s magnetosphere changes its position by an angle of approximately 26° over the orbital period of Jupiter, which induces seasonal variations in physical and optical characteristics of the planetary atmosphere. At the time close to the summer solstice for the northern hemisphere, Jupiter is in perihelion. Consequently, due to the significant orbital eccentricity, the energy influx into the atmosphere in the northern hemisphere is 21% larger than that in the southern one. This leads to the asymmetry in the meridional distribution of the reflectance of visible clouds. Analysis of the results of photometric observations of Jupiter for 1960–2019 showed that the ratio A_J = B_N/B_S adequately describes the activity of atmospheric processes on Jupiter, which shows periodic increases in brightness at tropical and temperate latitudes in the southern and northern regions by turn during one orbital period of Jupiter. The response of the atmosphere to changes in the irradiation by the Sun does not occur instantaneously but with some delay. The results of observations of Jupiter in the visible range in 1960–1995 and 2012–2019 show a synchronous delay of 3.4 year (τ_R ≈ 1.07 × 10⁸ s) in response to the 21% change in the irradiation of different hemispheres when the planet is orbiting the Sun. In 1995–2012, the discrepancy caused by the orbital motion of the planet was observed between the behavior of A_J, the solar activity index S_n, and Jupiter’s regime of exposure to the Sun. Variations associated with the influence of solar activity are mainly induced by significant changes in the ultraviolet radiation of the Sun. These changes first affect the energetics of the upper atmosphere of Jupiter, after which they are indirectly transmitted into the troposphere, sometimes reducing the value of the relaxation constant τ_R to ~2.5 years. Since 2012, the behavior of the time dependence of A_J, the index of solar activity, and the irradiation regime of Jupiter due to its orbital motion have become consistent again. The periodicity in changes of the photometric characteristics of the northern and southern hemispheres of Jupiter were also restored.

中文翻译：

---

从木星半球活动因子的变化估计氢-氦气辐射的弛豫时间

摘要

在木星的轨道周期内，木星磁层上的次太阳点以大约26°的角度改变其位置，这引起了行星大气物理和光学特性的季节性变化。在接近北半球的夏至时，木星正处于近日点。因此，由于明显的轨道偏心，北半球流入大气的能量比南半球大21％。这导致可见云的反射率的子午线分布不对称。对木星1960–2019年的光度观测结果的分析表明，比率A _J  =  B _N / B _S充分描述了木星的大气过程活动，这表明在木星的一个轨道周期内，南部和北部地区热带和温带纬度的亮度周期性增加。大气对太阳辐射变化的响应不是瞬间发生的，而是有一定的延迟。在可见光范围内木星观测在一九六○年至1995年和2012至2019年，结果显示为3.4年（τ一个同步延迟_[R ≈1.07×10个⁸响应于在不同的半球的照射的21％的变化或多个），当行星正在绕太阳运行。在1995-2012，行为之间观察到所引起的地球的轨道运动的差异是甲_Ĵ，太阳活动指数S _n和木星暴露于太阳的状态。与太阳活动影响有关的变化主要是由太阳紫外线辐射的显着变化引起的。这些变化首先影响木星的高层大气，之后它们被间接地发送到对流层的能量学，有时降低了松弛常数τ的值_[R至〜2.5年。自2012年起，的时间依赖性的行为甲_Ĵ，太阳活动的指标，和木星的照射政权由于其轨道运动再次成为一致。木星的北半球和南半球的光度特征变化的周期性也得以恢复。