Journal
ASTRONOMICAL JOURNAL
Volume 158, Issue 3, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-3881/ab2cd6
Keywords
planets and satellites: atmospheres; planets and satellites: gaseous planets; infrared: planetary systems
Categories
Funding
- European Research Council Consolidator Grant under the European Union's Horizon 2020 research and innovation program at the University of Leicester [723890]
- Royal Society Research Fellowship
- UK Science and Technology Facilities Council (STFC) [ST/N000749/1]
- National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program [NNX-08AE38A]
- STFC [ST/N000749/1, ST/L001306/1] Funding Source: UKRI
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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-mu m 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 1-4 bar 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-mu m-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 4-8 yr. 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 5 mu m brightness changes between the North Equatorial Belt and the South Equatorial Belt, suggesting a possible connection between the changes in these belts.
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