Great Red Spot

A false-color image of the Great Red Spot of Jupiter from Voyager 1. The white oval storm directly below the Great Red Spot has approximately the same diameter as the Earth. NASA image.

The Great Red Spot is a persistent anticyclonic storm on the planet Jupiter, 22° south of the equator, which has lasted for at least 186 years and possibly as long as 351 years or more.^[1][2] Storms such as this are not uncommon within the turbulent atmospheres of gas giants.

Observation history

Image of Jupiter by Pioneer 10 in 1974, showing a more solid-looking spot than when shown by Voyager 1 in 1979

The Great Red Spot (GRS) appears at first to be remarkably stable, and most sources concur that it has been continuously observed for 301 years. However, the situation is more complex than that; the present spot was first seen only after 1830 and well-studied only after a prominent apparition in 1879. A long gap separates its period of current study after 1830 from its seventeenth-century discovery; whether the original spot dissipated and re-formed, whether it faded, or even if the observational record was simply poor, are all unknown.^[3]

For example, its first sighting is often credited to Robert Hooke, who described a spot on the planet in May 1664; however, it is likely that Hooke's spot was in the wrong belt altogether (the North Equatorial Belt, versus the current Great Red Spot's location in the South Equatorial Belt). Much more convincing is Giovanni Cassini's description of a "permanent spot" the following year.^[4] With fluctuations in visibility, Cassini's spot was observed from 1665 to 1713; however, the 118-year observational gap makes the identity of the two spots inconclusive, and the older spot's shorter observational history and slower motion than the modern spot make their identity unlikely.^[5]

A minor mystery concerns a Jovian spot depicted in a 1711 canvas by Donato Creti, which is exhibited in the Vatican.^[6][7] Part of a series of panels in which different (magnified) heavenly bodies serve as backdrops for various Italian scenes, and all overseen by the astronomer Eustachio Manfredi for accuracy, Creti's painting is the first known to depict the GRS as red. Worth noting is the fact that no Jovian feature was officially described as red before the late 1800s.^[7]

A wider view of Jupiter and the Great Red Spot as seen from Voyager 1 in 1979

On February 25, 1979,^[8] when the Voyager 1 spacecraft was 9.2 million km (5.7 million miles) from Jupiter it transmitted the first detailed image of the Great Red Spot back to Earth. Cloud details as small as 160 km (100 miles) across were visible. The colorful, wavy cloud pattern seen to the left (west) of the Red Spot is a region of extraordinarily complex and variable wave motion.

Time-lapse sequence from the approach of Voyager 1 to Jupiter, showing the motion of atmospheric bands, and circulation of the Great Red Spot. NASA image.

At the start of 2004, the Great Red Spot had approximately half the longitudinal extent it had a century ago, when it reached a size of 40,000 km. At the present rate of reduction it would become circular by 2040, although this is unlikely because of the distortion effect of the neighboring jet streams. It is not known how long the spot will last, or whether the change is a result of normal fluctuations.^[9]

A smaller spot, designated Oval BA, formed recently (March 2000) from the merger of three white ovals,^[10] has turned reddish in color. Astronomers have christened it the Little Red Spot or Red, Jr. As of June 5, 2006, the Great Red Spot and Oval BA appeared to be approaching convergence.^[11] The storms pass each other about every two years, but the passings of 2002 and 2004 did not produce anything exciting. Amy Simon-Miller, of the Goddard Space Flight Center, predicted the storms would have their closest passing on July 4, 2006. Simon-Miller had been working with Imke de Pater and Phil Marcus of UC Berkeley, and a team of professional astronomers since April, studying the storms using the Hubble Space Telescope. On July 20, the two storms were photographed passing each other by the Gemini Observatory without converging.^[12] In May 2008 a third storm turned red.^[13]

The Great Red Spot should not be confused with the Great Dark Spot, a feature observed near the northern pole of Jupiter in 2000 with the Cassini–Huygens spacecraft.^[14] Note that a feature in the atmosphere of Neptune was also called the Great Dark Spot. The latter feature was imaged by Voyager 2 in 1989, and may have been an atmospheric hole rather than a storm and it was no longer present as of 1994 (although a similar spot had appeared farther to the north).

Structure

Approximate size comparison of Earth and the Great Red Spot.

The oval object rotates counterclockwise, with a period of about six Earth days^[15] or 14 Jovian days. The Great Red Spot's dimensions are 24–40,000 km west to east and 12–14,000 km south to north. It is large enough to contain two or three planets the size of Earth. The cloudtops of this storm are about 8 km above the surrounding cloudtops.

Infrared data has long indicated that the Great Red Spot is colder (and thus, higher in altitude) than most of the other clouds on the planet.^[16] However, recent infrared measurements of the upper atmosphere show far more heat above the GRS than the rest of the planet; "acoustic waves" rising from the storm have been proposed as an explanation for Jupiter's temperature.^[17]

Careful tracking of atmospheric features revealed the spot's counterclockwise circulation as far back as 1966, observations dramatically confirmed by the first time-lapse movies from the Voyager flybys.^[18] The spot is confined by a modest eastward jet stream to its south and a very strong westward one to its north.^[19] Though winds around the edge of the spot peak at ~120 m/s (430 km/h), currents inside it seem stagnant, with little inflow or outflow.^[20] The rotation period of the spot has decreased with time, perhaps as a direct result of its steady reduction in size.^[21]

Color animation of Jupiter's cloud motion.

The Great Red Spot's latitude has been stable for the duration of good observational records, typically varying by about a degree. Its longitude, however, is subject to constant variation.^[22][23] Because Jupiter does not rotate uniformly at all latitudes, astronomers have defined three different systems for defining the longitude. System II is used for latitudes of more than 10°, and was originally based on the average rotation rate of the Great Red Spot of 9h 55m 42s.^[24][25] Despite this, however, the spot has "lapped" the planet in System II at least 10 times since the early nineteenth century. Its drift rate has changed dramatically over the years and has been linked to the brightness of the South Equatorial Belt, and the presence or absence of a South Tropical Disturbance.^[26]

It is not known exactly what causes the Great Red Spot's reddish color. Theories supported by laboratory experiments suppose that the color may be caused by complex organic molecules, red phosphorus, or yet another sulphur compound, but a consensus has yet to be reached.

An animation of the Great Red Spot

The Great Red Spot varies greatly in hue, from almost brick-red to pale salmon, or even white. In fact, the spot occasionally "disappears", becoming evident only through the Red Spot Hollow, which is its niche in the South Equatorial Belt (SEB). Interestingly, its visibility is apparently coupled to the SEB; when the belt is bright white, the spot tends to be dark, and when it is dark, the spot is usually light. These periods when the spot is dark or light occur at irregular intervals; as of 1997, during the preceding 50 years, the spot was darkest in the periods 1961–1966, 1968–1975, 1989–1990, and 1992–1993.^[3]

Mechanics

As the hot gases that comprise Jupiter's atmosphere rise from lower levels to higher levels, eddies form and converge. As cooler gas falls back, the Coriolis force causes swirling motion across a region that may be many kilometers in diameter. These eddies can last for a long time, because there is no solid surface to provide friction and because colder cloud tops above the eddy allow little energy to escape by radiation. Once formed, such eddies are free to move, merging with or affecting the behavior of other storm systems in the atmosphere. It is theorized that this mechanism formed the Great Red Spot. According to this theory, many adjacent eddies are engulfed and merge with the spot, adding to the energy of the storm and contributing to its longevity.

Notes

References

• [Numerous authors] (1999). Beatty, Kelly J.; Peterson, Carolyn Collins; Chaiki, Andrew, eds. The New Solar System (4th ed.). Massachusetts: Sky Publishing Corporation. ISBN 0933346867. 
• Beebe, Reta (1997). Jupiter the Giant Planet (2nd ed.). Washington: Smithsonian Books. ISBN 1560986859. 
• Hockey, Thomas (1999). Galileo's Planet: Observing Jupiter Before Photography. Bristol, Philadelphia: Institute of Physics Publishing. ISBN 0750304480. 
• Peek, Bertrand M. (1981). The Planet Jupiter: The Observer's Handbook (Revised ed.). London: Faber and Faber Limited. ISBN 0571180264. 
• Rogers, John H. (1995). The Giant Planet Jupiter. Cambridge: Cambridge University Press. ISBN 0521410088. 
• Smith, B. A.; et al. (1979). "The Jupiter system through the eyes of Voyager 1". Science. 204: 951–957, 960–972. Bibcode:1979Sci...204..951S. doi:10.1126/science.204.4396.951. PMID 17800430. Retrieved 2007-06-14. 

External links

Wikimedia Commons has media related to Great Red Spot.

• Yang, Sarah (April 21, 2004). "Researcher predicts global climate change on Jupiter as giant planet's spots disappear". UC Berkeley News. Retrieved 2007-06-14. 
• Phillips, Tony (March 3, 2006). "Jupiter's New Red Spot". Science at NASA. Retrieved 2007-06-14. 
• Phillips, Tony (June 5, 2006). "Huge Storms Converge". Science at NASA. Retrieved 2007-06-14. 
• Youssef, Ashraf; Marcus, Philip S. (2003). "The dynamics of jovian white ovals from formation to merger". Icarus. 162 (1): 74–93. Bibcode:2003Icar..162...74Y. doi:10.1016/S0019-1035(02)00060-X. 
• Williams, Gareth P. (May 4, 2005). "NOAA Web Page". Geophysical Fluid Dynamics Laboratory. Retrieved 2007-07-21. 

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