摘要：Jupiter’s banded structure undergoes strong temporal variations, changing the visible and infrared appearance of the belts and zones in a complex and turbulent way through physical processes that are not yet understood. In this study, we use ground-based 5-μm infrared data captured between 1984 and 2018 by eight different instruments mounted on the Infrared Telescope Facility in Hawai’i and on the Very Large Telescope in Chile to analyze and characterize the long-term variability of Jupiter’s cloud-forming region at the 1–4bar pressure level. The data show a large temporal variability mainly at the equatorial and tropical latitudes, with a smaller temporal variability at mid-latitudes. We also compare the 5-μm-bright and -dark regions with the locations of the visible zones and belts, and we find that these regions are not always colocated, especially in the southern hemisphere. We also present Lomb–Scargle and Wavelet Transform analyses in order to look for possible periodicities of the brightness changes that could help us understand their origin and predict future events. We see that some of these variations occur periodically in time intervals of 4–8yr. The reasons for these time intervals are not understood, and we explore potential connections to both convective processes in the deeper weather layer and dynamical processes in the upper troposphere and stratosphere. Finally, we perform a Principal Component analysis to reveal a clear anticorrelation on the 5μm brightness changes between the North Equatorial Belt and the South Equatorial Belt, suggesting a possible connection between the changes in these belts.
关键词：planets and satellites: atmospheres;planets and satellites: gaseous planets;infrared: planetary systems
