Moist convective storms powered by the release of latent heat are a common feature in Jupiter’s atmosphere. Jovian convective storms form with a variety of spatial scales ranging from small short-lived storms affecting only their surroundings  to large long-lived storms that can develop into planetary-scale disturbances  following complex cycles of activity. These storms are an essential component in the atmospheric dynamics of the Gas Giants  and might be also an important element in the atmospheres of the Icy Giants .
Here we present new simulations of convective storms in Jupiter. An updated version of a three-dimensional Anelastic Model of Moist Convection [5-6] has been used to simulate the onset and initial development of convective storms in Jupiter’s atmosphere under different conditions to study under which ones the storms can develop. Three-dimensional models include the effects of the Coriolis force in the evolution of the storm and predict the motions developed in the storm, release of energy, cloud tops and a number of different features. The updated version of the model has an improved dynamical core increasing the stability and allowing the simulation of longer periods of time. We have tested different abundances of condensates, relative humidities and fractions of condensates carried by the storm.
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