Establishing the age and origin of Jupiter’s Great Red Spot

Research staff at the University of the Basque Country (UPV/EHU), the Universitat Politècnica de Catalunya—BarcelonaTech (UPC) and the Barcelona Supercomputing Center (CNS-BSC) have analyzed historical observations since the 17th century and developed numerical models to explain the longevity and nature of Jupiter’s Great Red Spot.

They have published the findings of their observations and numerical models in the journal Geophysical Research Letters.

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 color against the planet’s pale clouds make it an object that can be easily seen even with small telescopes.

Jupiter’s Great Red Spot is a huge anticyclonic vortex with winds traveling 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 the origin of the GRS 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 and named it the “Permanent Spot” (PS), since it was observed by him and other astronomers until 1713.

Astronomers subsequently lost track of it 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 various space missions that have visited the planet right up to the present day.

In the study, the authors first analyzed the evolution of its 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 Agustín Sánchez-Lavega, professor of physics at the UPV/EHU and who led this research.

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, “various 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,” explained Sánchez-Lavega.

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’s MareNostrum IV, part of the Spanish Supercomputing Network (RES), using two types of complementary models of the behavior 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 the opposite direction, 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 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 must have been observed and reported by the astronomers at the time,” said 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,” said Enrique García-Melendo, researcher in the UPC’s Department of Physics.

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 and reproduce the shrinkage of the GRS over time in order to find out, in greater detail, the physical mechanisms underlying its sustainability over time.

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 stabilize at a size limit at which it may last for many more years.