Investigating Temporal and Spatial Variation of Jupiter's Atmosphere with Radio Observations

TL;DR

This study analyzes Jupiter's atmospheric variability over time and space using radio observations from VLA and Juno, revealing frequency-dependent dynamics and scale differences in atmospheric features.

Contribution

It provides a comparative analysis of Jupiter's atmospheric variability across multiple radio frequencies and over several years, highlighting the spatial and temporal dynamics at different depths.

Findings

NEB shows the greatest brightness temperature variability.

Frequency bands 5 and 22 GHz exhibit the least variability.

Small-scale events are primarily observed at 10 and 15 GHz.

Abstract

We study the spatial and temporal variability in Jupiter's atmosphere by comparing longitude-resolved brightness temperature maps from the Very Large Array (VLA) radio observatory and NASA's Juno spacecraft Microwave Radiometer (MWR) taken between 2013 and 2018. Spatial variations in brightness temperature, as observed at radio wavelengths, indicate dynamics in the atmosphere as they trace spatial fluctuations in radio-absorbing trace gases or physical temperature. We use four distinct frequency bands, probing the atmosphere from the water cloud region at the lowest frequency to the pressures above the ammonia cloud deck at the highest frequency. We visualize the brightness temperature anomalies and trace dynamics by analyzing the shapes of brightness temperature anomaly distributions as a function of frequency in Jupiter's North Equatorial Belt (NEB), Equatorial Zone (EZ), and South Equatorial Belt (SEB). The NEB has the greatest brightness temperature variability at all frequencies, indicating that more extreme processes are occurring there than in the SEB and EZ. In general, we find that the atmosphere at 5 and 22 GHz has the least variability of the frequencies considered, while observations at 10 and 15 GHz have the greatest variability. When comparing the size of the features corresponding to the anomalies, we find evidence for small-scale events primarily at the depths probed by the 10 and 15 GHz observations. In contrast, we find larger-scale structures deeper (5 GHz) and higher (22 GHz) in the atmosphere.