  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.
