Researchers from the UPC, the BSC-CNS and the UPV/EHU establish the age and origin of Jupiter’s Great Red Spot
Researchers from the UPC’s Department of Physics Manel Soria, Enrique García-Melendo and Arnau Miró
Researchers Enrique García, Agustín Sánchez and Jon Legarreta in the office. Source: Fernando Gómez Larrea
Changes in the size of Jupiter’s Great Red Spot (GRS) over 134 years. Left, photograph taken on 14 October 1890 at the Lick Observatory (USA), slightly coloured to highlight the oval. Right, image obtained by the Hubble Space Telescope on 5 January 2024. Acknowledgements: BDIP-Observatoire Paris (left), HST/NASA/ESA/OPAL program (right).
Observation and simulation of the old GRS. Left, first photograph of Jupiter by A. A. Common from Ealing (London, England) on 3 September 1879. The GRS stands out prominently as a dark oval. Right, a numerical simulation model of the GRS observed that year superimposed on a recent image of Jupiter obtained by the Hubble Space Telescope (HST/NASA/ESA). The images are positioned according to the astronomical view (south at the top, east on the left). Acknowledgements: ©UPV-EHU/UPC.
Observation and simulation of the genesis of the GRS. Left, drawing of Jupiter produced by S. Swabe on 10 May 1851 showing the GRS area as a large clear oval with its edges marked by a dotted red line. Right, a numerical simulation model of a long slowly rotating cell produced by Jupiter’s winds superimposed on a recent image of the planet obtained by the Hubble Space Telescope (HST/NASA/ESA). The images are positioned according to the astronomical view (south at the top, east on the left). Acknowledgements: ©UPV-EHU/UPC.
Researchers from the UPC’s Department of Physics on the Terrassa Campus, the Barcelona Supercomputing Center – Centro Nacional de Supercomputación (BSC-CNS) and the University of the Basque Country (UPV/EHU) have analysed historical observations since the 17th century and have developed numerical models to explain the longevity and nature of this spectacular meteorological phenomenon in the atmosphere of the gas giant planet.
Jul 08, 2024
As a popular icon among objects in the Solar System, Jupiter’s Great Red Spot (GRS) is probably the best-known atmospheric structure. Its large size—right now its diameter is that of the Earth—and the contrast of its reddish colour against the planet’s pale clouds make it an object that can be easily seen even with small telescopes.
The GRS is a huge anticyclonic vortex with winds travelling at 450 km/h around its periphery. It is the largest and most long-lived vortex among all those existing in the atmospheres of the planets in the Solar System, but its age is a matter for debate and the mechanism that led to its formation remains obscure. Speculation about its origin dates back to the first telescopic observations made by the astronomer Giovanni Domenico Cassini, who in 1665 discovered a dark oval at the same latitude as the GRS. He named it the Permanent Spot (PS), since it was observed by him and other astronomers until 1713.
Track of it was subsequently lost for 118 years and it was not until 1831 and later years that S. Schwabe again observed a clear structure, roughly oval in shape and at the same latitude as the GRS, that can be regarded as the first observation of the current GRS, perhaps of a nascent GRS. Since then, the GRS has been observed regularly by means of telescopes and by the space missions that have visited the planet right up to the present day.
The study has been published in Geophysical Research Letters. Authors Agustín Sánchez-Lavega, Enrique García-Melendo, Jon Legarreta, Arnau Miró, Manel Soria and Kevin Ahrens-Velásquez firstly analysed the evolution of the GRS’s size over time, its structure and the movements of both meteorological formations, the former PS and the GRS. To do so, they used historical sources dating back to the mid-17th century, shortly after the invention of the telescope.
“From the measurements of sizes and movements we deduced that it is highly unlikely that the current GRS was the PS observed by G. D. Cassini. The PS probably disappeared sometime between the mid-18th and 19th centuries, in which case we can say that the longevity of the Red Spot now exceeds 190 years at least,” explained Sánchez-Lavega, a professor of Physics at the UPV/EHU and the study’s leader.
The Red Spot, which in 1879 was 39,000 km in size at its longest axis, has been shrinking to about the current 14,000 km and simultaneously becoming more rounded. What is more, since the 1970s several space missions have studied this meteorological phenomenon closely. Recently, several instruments on board the Juno mission in orbit around Jupiter have shown that the GRS is shallow and thin when compared to its horizontal dimension, as vertically it is about 500 km long.
Numerical simulations
To find out how this immense vortex could have formed, the UPV/EHU and UPC teams carried out numerical simulations on Spanish supercomputers, such as the BSC-CNS MareNostrum IV, part of the Spanish Supercomputing Network (RES). They used two types of complementary models of the behaviour of thin vortices in Jupiter’s atmosphere.
Predominating on the giant planet are intense wind currents that flow along the parallels alternating in their direction with the latitude. To the north of the GRS, winds blow in a westerly direction at speeds of 180 km/h while to the south, they blow in an easterly direction, at speeds of 150 km/h. This generates a huge north-south shear in wind speed, which is a basic ingredient enabling the vortex to grow inside it.
In the research a range of mechanisms were explored to explain the genesis of the GRS, including the eruption of a gigantic superstorm, similar to those rarely observed on the twin planet Saturn, or the merging of multiple smaller vortices produced by the wind shear. The results indicate that, although an anticyclone forms in both cases, it differs in terms of shape and dynamic properties from those of the present GRS.
“We also think that, if one of these unusual phenomena had occurred, it or its consequences in the atmosphere would have been observed and reported by the astronomers at the time,” noted Sánchez-Lavega.
In a third set of numerical experiments, the research team explored the generation of the GRS from a known instability in the winds that is thought to be capable of producing an elongated cell that encloses and traps them. Such a cell would be a proto-GRS, a nascent Red Spot, whose subsequent shrinkage would give rise to the compact and rapidly rotating GRS observed in the late 19th century.
The formation of large elongated cells has already been observed in the genesis of other major vortices on Jupiter. “In our simulations, supercomputers enabled us to discover that the elongated cells are stable when they rotate around the periphery of the GRS at the speed of Jupiter’s winds, as would be expected when they form because of this instability,” remarked Enrique García-Melendo, a researcher from the Department of Physics of the Universitat Politècnica de Catalunya - BarcelonaTech (UPC) and the Turbulence and Aerodynamics in Mechanical and Aerospace Engineering Research Group (TUAREG) at the Terrassa School of Industrial, Aerospace and Audiovisual Engineering (ESEIAAT).
Using two different types of numerical models, one at the UPV/EHU and the other at the UPC, the researchers concluded that, if the rotational speed of the proto-GRS is lower than that of the surrounding winds, the proto-GRS will break up, making the formation of a stable vortex impossible. And, if it is very high, the properties of the proto-GRS differ from those of the current GRS. Future research will aim to try to reproduce the shrinkage of the GRS over time in order to find out, in greater detail, the physical mechanisms underlying its sustainability. At the same time, it will try to predict whether the GRS will disintegrate and disappear when it reaches a size limit, as might have occurred to Cassini’s PS, or whether it will stabilise at a size limit at which it may last for many more years.
