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The Great Red Spot is a persistent anticyclonic storm on the planet Jupiter, 22° south of the equator, which has lasted at least 340 years. The storm is large enough to be visible through Earth-based telescopes. It was probably first observed by Giovanni Domenico Cassini, who described it around 1665.

This dramatic view of Jupiter's Great Red Spot and its surroundings was obtained by Voyager 1 on February 25, 1979, when the spacecraft was 9.2 million km (5.7 million miles) from Jupiter. Cloud details as small as 160 km (100 miles) across can be seen here. The colorful, wavy cloud pattern to the left of the Red Spot is a region of extraordinarily complex and variable wave motion. To give a sense of Jupiter's scale, the white oval storm directly below the Great Red Spot is approximately the same diameter as Earth.

The oval object rotates counterclockwise, with a period of about 6 days. The Great Red Spot's dimensions are 24-40,000 km × 12-14,000 km. It is large enough to contain two or three planets of Earth size. The cloud tops of this storm are about 8 km above the surrounding cloud tops.

Storms such as this are not uncommon within the turbulent atmospheres of gas giants. Jupiter also has white ovals and brown ovals, which are lesser unnamed storms. White ovals tend to consist of relatively cool clouds within the upper atmosphere. Brown ovals are warmer and located within the "normal cloud layer." Such storms can last hours or centuries.

Before the Voyager missions, astronomers were uncertain of the nature of Jupiter's Great Red Spot. Many believed it to be either a solid or a liquid feature on the planet's surface as this appears consistent with the observable turbulence patterns.

Recent examination of Jupiter's surface by a NASA research team using the Hubble telescope has shown that several smaller storms located near the Giant Red Spot have, in the last twelve months, amalgamated, increased in intensity and changed color from white to red.7 Further investigations on this Oval BA, nicknamed Red Spot Jr., using spectroscopy have been delayed due to the movement of Jupiter behind the Sun and it is yet to be verified if the phenomenon is caused by increased wind speed, comparable to those in the larger anomaly, drawing similar materials from deeper in the atmosphere and exposing them to sunlight. Given the relatively sudden development of Oval BA in the last 12 months and the as yet unconfirmed nature of the cause of either of the red spots, it is still open to speculation. It could be atmospheric activity drawing material up from closer to the planet's surface or it might be thermal activity on the surface throwing gases and debris upwards.

Planetary rings

This map of Jupiter's southern hemisphere shows its south pole at the center and equator at the edge. It was constructed from images taken by the Cassini spacecraft in December 2000.

Jupiter has a faint planetary ring system composed of smoke-like dust particles knocked from its moons by energetic meteor impacts. The innermost donut-shaped ring, called the halo, is almost as thick (20,000 km) as it is wide (22,800 km). This is followed by the thinnest and brightest main ring, which is made of dust from the satellites Adrastea and Metis. Metis orbits within its fluid Roche limit with Jupiter, and objects not rigidly attached to it may freely fall away from it and into Jupiter's gravitational field. Two wide gossamer rings encircle the main ring, originating from Thebe and Amalthea. Finally, there is a distant and very faint outer ring circling Jupiter backwards-retrograde of its spin. It is not known for certain where the material for this outer ring comes from, but it may be captured interplanetary dust.

Magnetosphere

Jupiter has a very large and powerful magnetosphere. In fact, if one could see Jupiter's magnetic field from Earth, it would appear five times as large as the full moon in the sky, despite being so much farther away. The magnetic field is generated by eddy currents (caused by a moving magnetic field intersecting a conductor) in Jupiter's metallic hydrogen core. This magnetic field collects a large flux of particle radiation in Jupiter's radiation belts, as well as producing a dramatic gas torus and flux tube associated with Io (one of Jupiter's moon). Jupiter's magnetosphere is the largest planetary structure in the solar system.8

The Pioneer probes confirmed that Jupiter's enormous magnetic field is 10 times stronger than Earth's and contains 20,000 times as much energy. The sensitive instruments aboard found that the Jovian magnetic field's "north" magnetic pole is at the planet's geographic south pole, with the axis of the magnetic field tilted 11 degrees from the Jovian rotation axis and offset from the center of Jupiter in a manner similar to the axis of the Earth's field. The Pioneers measured the bow shock of the Jovian magnetosphere to the width of 26 million kilometers (16 million miles), with the magnetic tail extending beyond Saturn's orbit.

The data showed that the magnetic field fluctuates rapidly in size on the sunward side of Jupiter because of pressure variations in the solar wind, an effect studied in further detail by the two Voyager spacecraft. It was also discovered that streams of high-energy atomic particles are ejected from the Jovian magnetosphere and travel as far as the orbit of the Earth. Energetic protons were found and measured in the Jovian radiation belt and electric currents were detected flowing between Jupiter and some of its moons, particularly Io.

Exploration of Jupiter

Since 1973, a number of automated spacecraft have visited Jupiter. Flights to other planets within the Solar System are accomplished at a cost in energy, which is described by the net change in velocity of the spacecraft, or delta-v. Reaching Jupiter from Earth requires a delta-v of 9.2 km/s,9 which is comparable to the 9.7 km/s delta-v needed to reach low Earth orbit.10 Fortunately, gravity assists through planetary flybys can be used to reduce the energy required to reach Jupiter, albeit at the cost of a significantly longer flight duration.

Pioneer flyby missions

Pioneer 10 flew past Jupiter in December of 1973, followed by Pioneer 11 exactly one year later. Pioneer 10 obtained the first ever close up images of Jupiter and the Galilean moons, studied its atmosphere, detected its magnetic field, observed its radiation belts and found that Jupiter is mainly liquid.

Voyager flyby missions

Voyager 1 took this photo of the planet Jupiter on January 24, 1979 while still more than 25 million miles (40 million kilometers) away.

Voyager 1 flew by in March 1979, followed by Voyager 2 in July of the same year. The Voyagers vastly improved the understanding of the Galilean moons and discovered Jupiter's rings. They also took the first close up images of the planet's atmosphere.11

Ulysses flyby mission

In February 1992, Ulysses solar probe performed a flyby of Jupiter at a distance of 409,000 km (6.3 Jovian radii). This critical maneuver was required for Ulysses to attain a polar orbit around the Sun. During this pass the probe conducted studies on Jupiter's magnetosphere. However, since there were no cameras on board the probe, no images were taken. In February 2004, the probe came again in the vicinity of Jupiter. This time the distance was much greater-about 240 million km.12

Galileo mission

So far, the only spacecraft to orbit Jupiter is the Galileo orbiter, which went into orbit around Jupiter on December 7, 1995. It orbited the planet for over seven years and conducted multiple flybys of all of the major Galilean moons and Amalthea. The spacecraft also witnessed the impact of Comet Shoemaker-Levy 9 into Jupiter as it approached the planet in 1994, giving a unique vantage point for this spectacular event. However, while the information gained about the Jovian system from the Galileo mission was extensive in its own right, its originally-designed capacity was limited by the failed deployment of its high-gain radio transmitting antenna.13

Jupiter as seen by the space probe Cassini. This is the most detailed global color portrait of Jupiter ever assembled.

An atmospheric probe was released from the spacecraft in July 1995. The probe entered the planet's atmosphere on December 7, 1995. It parachuted through 150 km of the atmosphere, collecting data for 57.6 minutes, before being crushed by the extreme pressure to which it was subjected. It would have melted and vaporized shortly thereafter. The Galileo orbiter itself experienced a more rapid version of the same fate when it was deliberately steered into the planet on September 21, 2003, at a speed of over 50 km/s, in order to avoid any possibility of it crashing into and possibly contaminating Europa, one of the Jovian moons.

Cassini flyby mission

In 2000, the Cassini probe, en route to Saturn, flew by Jupiter and provided some of the highest-resolution images ever taken of the planet. On December 19, 2000, the Cassini spacecraft, captured a very low resolution image of the moon Himalia, but it was too distant to show any surface details.

New Horizons flyby mission

The New Horizons probe and its Atlas V launcher lifted off from Pad 41 at Cape Canaveral Air Force Station, Florida, directly south of Space Shuttle Launch Complex 39, at 2:00 p.m. EST (1900 UTC) on January 19, 2006. New Horizons passed lunar orbit before midnight EST on the same day, and was scheduled to reach Jupiter in February 2007. It's plan was to pass through the Jupiter system at 21 km/s (47,000 mph), with closest approach to Jupiter occurring at approximately 06:00 UTC February 28, 2007.

The flyby was planned come within about 32 Jovian radii (3 Gm) of Jupiter and would be the center of a 4-month intensive observation campaign. New Horizons also has instruments built twenty years after Galileo's-particularly Galileo's cameras, which were evolved versions of the Voyager cameras which, in turn, were evolved Mariner cameras. Because of the much shorter distance from Jupiter to Earth, the communications link can transmit multiple loadings of the memory buffer. The mission will actually return more data from Jupiter than Pluto. Imaging of Jupiter began on September 4, 2006.

Future probes

NASA is planning a mission to study Jupiter in detail from a polar orbit. Named Juno, the spacecraft is planned to launch by 2010.

Because of the possibility of a liquid ocean on Jupiter's moon Europa, there has been great interest to study the icy moons in detail. A mission proposed by NASA was dedicated to study them. The JIMO (Jupiter Icy Moons Orbiter) was expected to be launched sometime after 2012. However, the mission was deemed too ambitious and its funding was canceled.

Natural satellites

Jupiter's 4 Galilean moons, in a composite image comparing their sizes and the size of Jupiter (Great Red Spot visible). From the top, they are: Callisto, Ganymede, Europa, and Io.A picture of Jupiter and its moon Io taken by the Hubble Space Telescope. The black spot is Io's shadow.

Jupiter has at least 63 moons. The four large moons, known as the "Galilean moons," are Io, Europa, Ganymede, and Callisto. The Galilean moons were first observed by Galileo on January 7, 1610.

Galilean moons

The orbits of Io, Europa, and Ganymede (the largest moon in the Solar System) form a pattern known as a Laplace resonance; for every four orbits that Io makes around Jupiter, Europa makes exactly two orbits and Ganymede makes exactly one. This resonance causes the gravitational effects of the three moons to distort their orbits into elliptical shapes, since each moon receives an extra tug from its neighbors at the same point in every orbit it makes.

The tidal force from Jupiter, on the other hand, works to circularize their orbits. This constant tug of war causes regular flexing of the three moons' shapes, Jupiter's gravity stretches the moons more strongly during the portion of their orbits that are closest to it and allowing them to spring back to more spherical shapes when they're farther away. This flexing causes tidal heating of the three moons' cores. This is seen most dramatically in Io's extraordinary volcanic activity, and to a somewhat less dramatic extent in the geologically young surface of Europa indicating recent resurfacing.

The Galilean moons, compared to Earth's moon Luna
Name

(Pronunciation key)

Diameter
(km)
Mass
(kg)
Orbital radius (km)Orbital period (days)
Ioeye'-oe3643
(105% Luna)
8.9×1022
(120% Luna)
421 700
(110% Luna)
1.77
(6.5% Luna)
Europaew-roe'-pə3122
(90% Luna)
4.8×1022
(65% Luna)
671 034
(175% Luna)
3.55
(13% Luna)
Ganymedegan'-ə-meed5262
(150% Luna)
14.8×1022
(200% Luna)
1 070 412
(280% Luna)
7.15
(26% Luna)
Callistokə-lis'-toe4821
(140% Luna)
10.8×1022
(150% Luna)
1 882 709
(490% Luna)
16.69
(61% Luna)

Classification of Jupiter's moons

Before the discoveries of the Voyager missions, Jupiter's moons were arranged neatly into four groups of four. Since then, the large number of new small outer moons has complicated this picture. There are now thought to be six main groups, although some are more distinct than others. A basic division is between (a) the eight inner regular moons with nearly circular orbits near the plane of Jupiter's equator, which are believed to have formed with Jupiter; and (b) an unknown number of small, irregular moons, with elliptical and inclined orbits, which are believed to be captured asteroids or fragments of captured asteroids.

Europa, one of Jupiter's many moons.
  1. Regular moons:
    1. The inner group of four small moons all have diameters of less than 200 km, orbit at radii less than 200,000 km, and have orbital inclinations of less than half a degree.
    2. The four Galilean moons, discovered by Galileo Galilei and Simon Marius, orbit between 400,000 and 2,000,000 km, and include some of the largest moons in the solar system.
  2. Irregular moons:
    1. Themisto is in a group of its own, orbiting halfway between the Galilean moons and the next group.
    2. The Himalia group is a tightly clustered group of moons with orbits around 11,000,000-12,000,000 km from Jupiter.
    3. Carpo is another isolated case; at the inner edge of the Ananke group, it revolves in the direct sense.
    4. The Ananke group is a group with rather indistinct borders, averaging 21,276,000 km from Jupiter with an average inclination of 149 degrees.
    5. The Carme groupis a fairly distinct group that averages 23,404,000 km from Jupiter with an average inclination of 165 degrees.
    6. The Pasiphaë group is a dispersed and only vaguely distinct group that covers all the outermost moons.

It is thought that each group of outer moons may have a common origin, perhaps as a larger moon or captured body that broke up.

Life on Jupiter

It is considered highly unlikely that there is any Earth-like life on Jupiter, as there is little water in the atmosphere and any possible solid surface deep within Jupiter would be under extraordinary pressures. However, in 1976, before the Voyager missions, Carl Sagan hypothesized (with Edwin Ernest Salpeter) that ammonia-based life could evolve in Jupiter's upper atmosphere. Sagan and Salpeter based this hypothesis on the ecology of terrestrial seas, which have simple photosynthetic plankton at the top level, fish at lower levels feeding on these creatures, and marine predators that hunt the fish. The Jovian equivalents Sagan and Salpeter hypothesized were "sinkers," "floaters," and "hunters." The "sinkers" would be plankton-like organisms which fall through the atmosphere, existing just long enough that they can reproduce in the time they are kept afloat by convection. The "floaters" would be giant bags of gas functioning along the lines of hot air balloons, using their own metabolism (feeding off sunlight and free molecules) to keep their gas warm. The "hunters" would be almost squid-like creatures, using jets of gas to propel themselves into "floaters" and consume them.14

This diagram shows the Trojan Asteroids in Jupiter's orbit, as well as the main asteroid belt.

Trojan asteroids

In addition to its moons, Jupiter's gravitational field controls numerous asteroids which have settled into regions known as "Lagrangian points" preceding and following Jupiter in its orbit around the Sun. They are called Trojan asteroids and are divided into Greek and Trojan "camps," to commemorate the Iliad. The first of these, 588 Achilles, was discovered by Max Wolf in 1906. Since then, hundreds more have been discovered. The largest among them is 624 Hektor.

Trojan asteroids are dominated by so-called D-type asteroids, which are believed to be abundant in hydrous minerals, carbon, and organics.15 However, unlike the D-type asteroids in the main asteroid belt, remote observations indicate no sign of water on Trojan asteroids. This lack of water may be due to heavy space weathering, for these asteroids are stable in orbit and their surfaces are believed to be much older than those in the main belt.

Cometary impact

Aftermath of impact of a cometary fragment. The dark scars visible on the cloudtops were larger than Earth itself.

During the period July 16 to 22, 1994, over twenty fragments from the comet Shoemaker-Levy 9 hit Jupiter's southern hemisphere, providing the first direct observation of a collision between two solar system objects. It is thought that due to Jupiter's large mass and location near the inner solar system it receives the most frequent comet impacts of the solar system's planets. Shoemaker-Levy 9 split into smaller pieces due to Jupiter's tidal force before the impact.

Footnotes

  1. ↑ Working Group on Extrasolar Planets: Definition of a "Planet," IAU position statement. Retrieved June 8, 2007.
  2. ↑ J. Sommeria, S.D. Meyers, and H.L. Swinney H.L., "Laboratory simulation of Jupiter's Great Red Spot," Nature, 331, (1988): 689-693.
  3. ↑ NASA, Jupiter's New Red Spot. Retrieved June 8, 2007.
  4. ↑ Ellie Crystal's Metaphysical and Science Website, Jupiter. Retrieved June 8, 2007.
  5. ↑ D. Gautier, et al, "The helium abundance of Jupiter from Voyager", Journal of Geophysical Research, 86, (1981): 8713-8720 (Abstract).
  6. ↑ S.J. Kim, J. Caldwell, A.R. Rivolo, R. Wagner, "Infrared Polar Brightening on JupiterIII. Spectrometry from the Voyager 1 IRIS Experiment," Icarus, 64, (1984): 233-248.
  7. ↑ A. Simon-Miller, et al, "Jupiter's White Oval turns red," Icarus 185, (2006): 558-562.
  8. ↑ The Astrophysics Spectator, "Jupiter's Magnetosphere." Retrieved June 8, 2007.
  9. ↑ Project Galileo Homepage, Galileo FAQ. Retrieved June 8, 2007.
  10. ↑ Rockets and Space Transportation, Delta V in the Solar System. Retrieved June 8, 2007.
  11. ↑ NASA Jet Propulsion Laboratory, Jupiter. Retrieved June 8, 2007.
  12. ↑ K. Chan, E. S. Paredes, M. S. Ryne, "Ulysses Attitude and Orbit Operations: 13+ Years of International Cooperation," American Institute of Aeronautics and Astronautics, (2004).
  13. ↑ NASA Jet Propulsion Laboratory, Galileo: Journey to Jupiter. Retrieved June 8, 2007.
  14. ↑ Encyclopedia of Astrobiology, Astronomy & Spaceflight //www.daviddarling.info/encyclopedia/J/Jupiterlife.html Life On Jupiter. Retrieved June 8, 2007.
  15. ↑ T. Hiroi, M.E. Zolensky, and C.M. Pieters, "The Tagish Lake meteorite: A possible sample from a D-type asteroid," Science, 293, (2001): 2234-2236.

References

  • Bagenal, Fran, Timothy E. Dowling, William B. McKinnon (Eds.) (2007). Jupiter: The Planet, Satellites, and Magnetosphere. Cambridge, UK; New York, NY: Cambridge University Press, New Ed Edition. ISBN 978-0521035453
  • Beebe, Reta (2002). Jupiter: The Giant Planet (second edition). Washington, DC: Smithsonian Institute Press. ISBN 1560986859
  • Seymour, Simon (1992). Our Solar System. New York, NY: HarperCollins. ISBN 978-0688099923
  • Spangenburg, Ray, and Kit Moser (2002). A Look at Jupiter (Out of This World). London, UK: Franklin Watts. ISBN 0531165639
Carme groupS/2003 J 17 · S/2003 J 10 · Pasithee · Chaldene · Arche · Isonoe · Erinome · Kale · Aitne · Taygete · S/2003 J 9 · Carme · S/2003 J 5 · S/2003 J 19 · Kalyke · Eukelade · KallichorePasiphaë groupEurydome · S/2003 J 23 · Hegemone · Pasiphaë · Sponde · Cyllene · Megaclite · S/2003 J 4 · Callirrhoe · Sinope · Autonoe · Aoede · KoreS/2003 J 2Rings of Jupiter
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