木星南温带大尺度气旋内对流扰动的观测和数值模拟
Observations and numerical modelling of a convective disturbance in a large-scale cyclone in Jupiter's South Temperate Belt
摘要：
木星上的湿对流风暴频繁发展，可以引发不同尺度的大气活动，从局部风暴到行星尺度的扰动，包括局限于较大气象系统内的对流活动。2018年2月，木星南温带（行星中心纬度从-23 $^{\circ}$到-29.5 $^{\circ}$）爆发了一系列对流风暴。这场风暴发生在一个被称为STB幽灵的细长气旋区域内，靠近大型反气旋椭圆形BA，导致风暴产生的云层被限制在气旋内。最初的风暴只持续了几天，但它们产生了大量持久的湍流。它们还产生了黑暗的特征，可能部分没有云，在第一周围绕气旋循环。随后的活动发展了数月，并形成了两个主要结构，其中一个与椭圆形BA密切互动，另一个被驱逐到西部。在这里，我们提出了一个研究这种气象活动的基础上提供的日常观测业余社会，补充观测从PlanetCam UPV/EHU在卡拉尔阿尔托天文台，哈勃太空望远镜和朱诺号航天器上的朱诺相机。我们还进行了数值模拟与EPIC大气环流模式再现所观察到的现象。成功的模拟需要一个复杂的相互作用之间的幽灵，对流爆发和椭圆形BA，他们表明，水湿对流的来源，最初的风暴。与其他可以在可见光和甲烷吸收带图像中观察到的潮湿对流风暴进行简单的尺度比较，强烈表明大多数这些风暴是由水冷凝而不是氨驱动的。
英文摘要：
Moist convective storms in Jupiter develop frequently and can trigger atmospheric activity of different scales, from localized storms to planetary-scale disturbances including convective activity confined inside a larger meteorological system. In February 2018 a series of convective storms erupted in Jupiter's South Temperate Belt (STB) (planetocentric latitudes from -23$^{\circ}$ to -29.5$^{\circ}$). This occurred inside an elongated cyclonic region known popularly as the STB Ghost, close to the large anticyclone Oval BA, resulting in the clouds from the storms being confined to the cyclone. The initial storms lasted only a few days but they generated abundant enduring turbulence. They also produced dark features, possibly partially devoid of clouds, that circulated around the cyclone over the first week. The subsequent activity developed over months and resulted in two main structures, one of them closely interacting with Oval BA and the other one being expelled to the west. Here we present a study of this meteorological activity based on daily observations provided by the amateur community, complemented by observations obtained from PlanetCam UPV/EHU at Calar Alto Observatory, the Hubble Space Telescope and by JunoCam on the Juno spacecraft. We also perform numerical simulations with the EPIC General Circulation Model to reproduce the phenomenology observed. The successful simulations require a complex interplay between the Ghost, the convective eruptions and Oval BA, and they demonstrate that water moist convection was the source of the initial storms. A simple scale comparison with other moist convective storms that can be observed in the planet in visible and methane absorption band images strongly suggests that most of these storms are powered by water condensation instead of ammonia.
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