Surprises in the First 40-Year Tracking of Jupiter’s Temperature Variability

Surveillance of Jupiter’s tropospheric temperatures for over 40 years has yielded unexpected results. Orton et al. (2022 Nature Astronomy) have discovered variabilities that differ from Jupiter’s weak seasonal cycles, and connections between temperature variability at very distant latitudes.
Published in Astronomy
Surprises in the First 40-Year Tracking of Jupiter’s Temperature Variability

Exploring the atmospheric conditions associated with Jupiter’s colorful banded appearance has been a scientific challenge.  Chief among the properties to be determined is temperature, which is intimately tied to atmospheric dynamics, cloud formation, and chemistry. The Pioneer 10 and 11 spacecraft in the early 1970s revealed temperatures varying generally from warmer air over visibly darker bands to cooler air over lighter bands. But the visible banding was known to change over time, so the relationship between variability of temperatures and other properties of the atmosphere remained unknown.

Questions about time variability were pursued with observations of Jupiter’s thermal emission from ground-based telescopes. The relevant technology changed substantially over time, starting with temperature maps made using repeated north-south scans over the center of Jupiter’s disk as it rotated. Subsequent advances enabled 2-dimensional raster-scanned maps, followed by 2-dimensional cameras. This ground-based record established a link between the 1979 Voyager and 2001 Cassini observations, two decades apart. They also provided temperature maps to supplement the limited regions covered by the Galileo mission in 1995-2003 and the reconnaissance of Jupiter’s deeper atmosphere by Juno since 2016. Our challenge was to compare these thermal observations from vastly different instruments.

Image of Jupiter using a filter centered near 18 µm, taken by the COMICS instrument at the Subaru Telescope atop Maunakea, Hawaii, on 2019 May 27. Brighter and darker areas designate warmer and cooler regions, respectively, around 330 mbars of pressure in the upper troposphere.

The first study of variability of Jupiter’s tropospheric temperatures relied on the analysis of 1- and 2-dimensional scans of its disk covering 1980 – 1990, later extended to 2001.  That study hinted that stratospheric temperatures at low latitudes varied the opposite way from tropospheric temperatures. The limited coverage, barely a Jovian year (11.9 Earth years), made it impossible to make a robust distinction between seasonal and non-seasonal variability.

Our new study greatly extends this work, succeeding in providing the first measurement of temperatures in Jupiter’s upper troposphere covering over 40 years of scanning, mapping and imaging - over three Jovian orbits, making possible distinctions between seasonal and non-seasonal variability. We used data taken with the two most common filters among all the observations.  From them we derived the temperature at a single level in Jupiter’s upper troposphere at 330 mbars of pressure. We also limited our study to within 30° of latitude from the equator in order to preserve the highest spatial resolution of all the observations.

What we found was very unexpected. Various periodicities affecting different temperate to tropical latitudes are evident in the figure below.  The 10-14 year periodicities are intriguingly close to Jupiter’s 11.9-year orbital period but are much larger than models of seasonal variability. The 4- and 8-9 year periods suggest a relationship with the variability of stratospheric temperatures; a closer comparison with the variability of brightness temperatures emitted from the stratosphere, a proxy for ~10-mbar temperatures, shows an anticorrelation that is consistent with a descending thermal wave, representing a “top-down” control of tropospheric temperatures at low latitudes. The 7-year periodicity suggests a relationship with disruption with the same cadence, but limited to the equator.

Difference between the derived 330-mbar temperatures and their longitudinal mean (left) and the corresponding power spectra at each latitude, enhanced to visualize faint but important features (right). The white box bounds the latitude and period of  4.3±0.5 years, the dark orange box 7.4±0.6 years, the blue box 8.3±1.0 years. The light orange boxes identify a spread of 10.4-11.7 ±1.0 years in the north and a period of 10.5±1.0 years in the south. The yellow boxes identify a period spread of 10.3 – 11.6 ±1.5 years in the north and 11.4-13.1±1.0 years in the south. The red box identifies a broad peak period spread of 11.6-13.2 ±1.0 years. There are no significant periods longer than 14 years

Possibly the most surprising of all was the presence of anticorrelations of temperature variability between the northern and southern hemispheres that peaked at specific longitudes: 16°, 22° and 30° from the equator; the anticorrelations at 16° and 30° are evident in the blue vs red lines in the figure below. The oscillations at 16° north and south of the equator could be related to deep-seated cylinders parallel to the rotation axis, but such cylinders at 22° and 30° from the equator would intersect an non-transmitting region of metallic hydrogen. So if the connection cannot be via the deep atmosphere, then maybe Jupiter’s atmosphere transmits information horizontally over vast distances, potentially via a spectrum of atmospheric waves.  This behavior is suggestive of similarly teleconnected patterns of variability between the Earth’s two hemispheres, such as the El Nino Southern Oscillation (ENSO) or the North Atlantic Oscillation (NAO), which themselves are not well understood.

A correspondence between the darkening of prominent bands just north and south of the equator appeared to be consistent with the removal of aerosols by heating and sublimation during episodes of warmer temperatures; similarly their brightening was consistent with and the establishment of light-colored aerosols by cooling and freezing during episodes of colder temperatures.

Retrieved 330-mbar temperatures (A) at the equator, (B) 16° from the equator, and (C) 30° from the equator. Filled circles show the temperatures derived at each date of measurement, and solid lines indicate temperatures retrieved. Open circles at the equator denote the poorer spatial resolution of these data. Asterisks denote corresponding 330-mbar temperature differences derived by the Voyager-1 IRIS instrument in 1978 and the Cassini CIRS instrument in 2001.

The natural patterns revealed by our long-term study of Jupiter’s atmospheric variability might one day enable a Jovian weather forecast; but before we reach that goal, we must explain the processes driving such patterns.  Beneath all of Jupiter’s highly variable, ever-changing colorful cloud decks are predictable periodic oscillations, teleconnecting regions tens of thousands of kilometers apart.  These may provide a new window onto the processes at work in Jupiter’s hidden interior.  Reproducing these natural climate cycles will be a key challenge for future Jovian atmospheric models.

Please sign in or register for FREE

If you are a registered user on Research Communities by Springer Nature, please sign in

Subscribe to the Topic

Astronomy, Cosmology and Space Sciences
Physical Sciences > Physics and Astronomy > Astronomy, Cosmology and Space Sciences

Related Collections

With collections, you can get published faster and increase your visibility.

Progress towards the Sustainable Development Goals

The year 2023 marks the mid-point of the 15-year period envisaged to achieve the Sustainable Development Goals, targets for global development adopted in September 2015 by all United Nations Member States.

Publishing Model: Hybrid

Deadline: Ongoing

Wind, water and dust on Mars

In this Collection, we bring together recent work, and invite further contributions, on the nature and characteristics of the Martian surface, the processes at play, and the environmental conditions both in the present-day and in the distant past.

Publishing Model: Hybrid

Deadline: Ongoing