Modeling Jupiter’s Convective Plumes: First Results from a High-Resolution 3D Cloud-Resolving Model

Jupiter's turbulent atmosphere is host to intense convective and storm activity. These phenomena range from towering small-scale plumes reaching 50 km in height to massive mesoscale complexes spanning thousands of kilometers (Palotai et al., 2023). Often accompanied by lightning, these storms are mainly powered by the latent heat released from water condensation and are triggered by the planet's internal heat flux (Ingersoll et al., 2000; Palotai et al., 2023) and/or local dynamics (Sankar et al., 2025). Understanding the mechanisms that trigger and shape these convective events has motivated the development of various Cloud-Resolving Models (CRMs) (Hueso & Sánchez-Lavega, 2001; Sugiyama et al., 2014; Li & Chen, 2019). Continuing to improve these models is crucial for interpreting current observations from the Juno spacecraft (Fletcher et al., 2020; Read, 2024) and preparing for the upcoming JUICE mission.

To gain insight into Jupiter's deep moist convection, we utilize a 3D Cloud Resolving Model (CRM). The non-hydrostatic dynamical core of the model is inherited from the terrestrial Weather Research and Forecasting (WRF) model. It has been coupled to the physics of the Planetary Climate Model (PCM) suite for various planetary atmospheres, including Mars, Venus, Titan, the Ice Giants (Clément et al., 2024) and temperate exoplanets (Leconte et al., 2024). For Jupiter, our model covers a localized domain of a few hundred kilometers at a high spatial resolution (~1-2 km in both horizontal and vertical dimensions), allowing us to explicitly resolve individual small-scale convective plumes. For initial conditions, we first run a 1D radiative-convective version of the model (Guerlet et al., 2020) until a steady state is reached (after ~25 Jovian years). The resulting temperature, pressure, and humidity profiles are then utilized as the background atmospheric sounding to initialize the 3D simulations (Clément et al., 2024). Note that we currently include the condensation/precipitation/evaporation of water only, and not the other condensates.

We conduct benchmarking tests to validate the model's performance under Jovian conditions. This includes evaluating the sensitivity of the model to various grid configurations (such as vertical resolution and model top placement) to mitigate numerical artifacts and ensure dynamic stability. Preliminary 3D simulations successfully showcase the spontaneous formation of water storms driven by latent heat release of water.  We report the development of distinct convective structures, characterized by strong, localized updrafts (reaching vertical velocities on the order of ~50-100 m/s) and precipitation-driven downdrafts.

Following the finalization of the benchmark test cases, this CRM is planned to be used to systematically investigate the influence of varying atmospheric forcing on storm properties. We will explore how different internal heat fluxes, insolation levels, and deep-water abundances affect the horizontal and vertical extent, intensity, frequency, and lifetime of convective plumes. Ultimately, this local-scale modeling will serve as a stepping stone for future regional-scale studies, helping to parameterize the effect of small-scale storms on Jupiter's large-scale circulation and alternating zonal winds in Global Circulation Models (GCMs).

 

References

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