Jupiter

Jupiter is the fifth planet from the Sun and is the largest planet in the solar system. If Jupiter were hollow, more than one thousand Earths could fit inside. It also contains two and a half times the mass of all the other planets combined. It has a mass of 1.9 x 10²⁷ kg and is 142,800 kilometers (88,736 miles) across the equator. Jupiter possesses 62 known satellites. The four largest are Callisto, Europa, Ganymede and Io, and were named after Galileo Galilei who observed them as long ago as 1610. The German astronomer Simon Marius claimed to have seen the moons around the same time, but he did not publish his observations and so Galileo is given the credit for their discovery.

Jupiter has a very faint ring system, but is totally invisible from the Earth. (The rings were discovered in 1979 by Voyager 1.) The atmosphere is very deep, perhaps comprising the whole planet, and is somewhat like the Sun. It is composed mainly of hydrogen and helium, with small amounts of methane, ammonia, water vapor and other compounds. At great depths within Jupiter, the pressure is so great that the hydrogen atoms are broken up and the electrons are freed so that the resulting atoms consist of bare protons. This produces a state in which the hydrogen becomes metallic.

Colorful latitudinal bands, atmospheric clouds and storms illustrate Jupiter's dynamic weather systems. The cloud patterns change within hours or days. The Great Red Spot is a complex storm moving in a counter-clockwise direction. At the outer edge, material appears to rotate in four to six days; near the center, motions are small and nearly random in direction. An array of other smaller storms and eddies can be found through out the banded clouds.

Auroral emissions, similar to Earth's northern lights, were observed in the polar regions of Jupiter. The auroral emissions appear to be related to material from Io that spirals along magnetic field lines to fall into Jupiter's atmosphere. Cloud-top lightning bolts, similar to superbolts in Earth's high atmosphere, were also observed.

Jupiter's Ring

Unlike Saturn's intricate and complex ring patterns, Jupiter has a simple ring system that is composed of an inner halo, a main ring and a Gossamer ring. To the Voyager spacecraft, the Gossamer ring appeared to be a single ring, but Galileo imagery provided the unexpected discovery that Gossamer is really two rings. One ring is embedded within the other. The rings are very tenuous and are composed of dust particles kicked up as interplanetary meteoroids smash into Jupiter's four small inner moons Metis, Adrastea, Thebe, and Amalthea. Many of the particles are microscopic in size.

The innermost halo ring is toroidal in shape and extends radially from about 92,000 kilometers (57,000 miles) to about 122,500 kilometers (76,000 miles) from Jupiter's center. It is formed as fine particles of dust from the main ring's inner boundary 'bloom' outward as they fall toward the planet. The main and brightest ring extends from the halo boundary out to about 128,940 kilometers (80,000 miles) or just inside the orbit of Adrastea. Close to the orbit of Metis, the main ring's brightness decreases.

The two faint Gossamer rings are fairly uniform in nature. The innermost Amalthea Gossamer ring extends from the orbit of Adrastea out to the orbit of Amalthea at 181,000 kilometers (112,000 miles) from Jupiter's center. The fainter Thebe Gossamer ring extends from Amalthea's orbit out to about Thebe's orbit at 221,000 kilometers (136,000 miles).

Jupiter's rings and moons exist within an intense radiation belt of electrons and ions trapped in the planet's magnetic field. These particles and fields comprise the jovian magnetosphere or magnetic environment, which extends 3 to 7 million kilometers (1.9 to 4.3 million miles) toward the Sun, and stretches in a windsock shape at least as far as Saturn's orbit - a distance of 750 million kilometers (466 million miles).

Jupiter Statistics
Mass (kg)	1.900e+27
Mass (Earth = 1)	3.1794e+02
Equatorial radius (km)	71,492
Equatorial radius (Earth = 1)	1.1209e+01
Mean density (gm/cm^3)	1.33
Mean distance from the Sun (km)	778,330,000
Mean distance from the Sun (Earth = 1)	5.2028
Rotational period (days)	0.41354
Orbital period (days)	4332.71
Mean orbital velocity (km/sec)	13.07
Orbital eccentricity	0.0483
Tilt of axis (degrees)	3.13
Orbital inclination (degrees)	1.308
Equatorial surface gravity (m/sec^2)	22.88
Equatorial escape velocity (km/sec)	59.56
Visual geometric albedo	0.52
Magnitude (Vo)	-2.70
Mean cloud temperature	-121°C
Atmospheric pressure (bars)	0.7
Atmospheric composition Hydrogen Helium	90% 10%

Animations of Jupiter

Views of Jupiter

Jupiter
This image was taken by NASA's Hubble Space Telescope on February 13, 1995. The image provides a detailed look at a unique cluster of three white oval-shaped storms that lie southwest (below and to the left) of Jupiter's Great Red Spot. The appearance of the clouds, in this image, is considerably different from their appearance only seven months earlier. These features are moving closer together as the Great Red Spot is carried westward by the prevailing winds while the white ovals are swept eastward.

The outer two of the white storms formed in the late 1930s. In the centers of these cloud systems the air is rising, carrying fresh ammonia gas upward. New, white ice crystals form when the upwelling gas freezes as it reaches the chilly cloud top level where temperatures are -130°C (-200°F). The intervening white storm center, the ropy structure to the left of the ovals, and the small brown spot have formed in low pressure cells. The white clouds sit above locations where gas is descending to lower, warmer regions.

Cassini Jupiter Portrait

This true color mosaic of Jupiter was constructed from images taken by the Cassini spacecraft on December 29, 2000, during its closest approach to the giant planet at a distance of approximately 10 million kilometers (6.2 million miles).

It is the most detailed global color portrait of Jupiter ever produced; the smallest visible features are approximately 60 kilometers (37 miles) across. The mosaic is composed of 27 images: nine images were required to cover the entire planet in a tic-tac-toe pattern, and each of those locations was imaged in red, green, and blue to provide true color. Although Cassini's camera can see more colors than humans can, Jupiter's colors in this new view look very close to the way the human eye would see them.

Everything visible on the planet is a cloud. The parallel reddish-brown and white bands, the white ovals, and the large Great Red Spot persist over many years despite the intense turbulence visible in the atmosphere. The most energetic features are the small, bright clouds to the left of the Great Red Spot and in similar locations in the northern half of the planet. These clouds grow and disappear over a few days and generate lightning. Streaks form as clouds are sheared apart by Jupiter's intense jet streams that run parallel to the colored bands. The prominent dark band in the northern half of the planet is the location of Jupiter's fastest jet stream, with eastward winds of 480 kilometers (300 miles) per hour. Jupiter's diameter is eleven times that of Earth, so the smallest storms on this mosaic are comparable in size to the largest hurricanes on Earth.

Unlike Earth, where only water condenses to form clouds, Jupiter's clouds are made of ammonia, hydrogen sulfide, and water. The updrafts and downdrafts bring different mixtures of these substances up from below, leading to clouds at different heights. The brown and orange colors may be due to trace chemicals dredged up from deeper levels of the atmosphere, or they may be byproducts of chemical reactions driven by ultraviolet light from the Sun. Bluish areas, such as the small features just north and south of the equator, are areas of reduced cloud cover, where one can see deeper. (Courtesy NASA/JPL/Space Science Institute)

The Interior of Jupiter
This picture illustrates the internal structure of Jupiter. The outer layer is primarily composed of molecular hydrogen. At greater depths the hydrogen starts resembling a liquid. At 10,000 kilometers below Jupiter's cloud top liquid hydrogen reaches a pressure of 1,000,000 bar with a temperature of 6,000° K. At this state hydrogen changes into a phase of liquid metallic hydrogen. In this state, the hydrogen atoms break down yeilding ionized protons and electrons similar to the Sun's interior. Below this is a layer dominated by ice where "ice" denotes a soupy liquid mixture of water, methane, and ammonia under high temperatures and pressures. Finally at the center is a rocky or rocky-ice core of up to 10 Earth masses. (Copyright Calvin J. Hamilton)

Thin Crescent Image of Jupiter
This thin crescent picture of Jupiter was created from a photomosaic of images Galileo took on its C9 orbit. It is made from Near Infrared and Violet images, with an artificial green image produced from the other two. (Courtesy of Ted Stryk)

Nordic Optical Telescope
This image of Jupiter was taken with the 2.6 meter Nordic Optical Telescope, located at La Palma, Canary Islands. It is a good example of the best imagery that can be obtained from earth based telescopes. (c) Nordic Optical Telescope Scientific Association (NOTSA).

Jupiter with Satellites Io and Europa
Voyager 1 took this photo of Jupiter and two of its satellites (Io, left, and Europa, right) on Feb. 13, 1979. In this view, Io is about 350,000 kilometers (220,000 miles) above Jupiter's Great Red Spot, while Europa is about 600,000 kilometers (373,000 miles) above Jupiter's clouds. Jupiter is about 20 million kilometers (12.4 million miles) from the spacecraft at the time of this photo. There is evidence of circular motion in Jupiter's atmosphere. While the dominant large scale motions are west-to-east, small scale movement includes eddy like circulation within and between the bands. (Courtesy NASA/JPL)

Satellite Footprints Seen in Jupiter Aurora
In this Hubble Space Telescope picture, a curtain of glowing gas is wrapped around Jupiter's north pole like a lasso. This curtain of light, called an aurora, is produced when high-energy electrons race along the planet's magnetic field and into the upper atmosphere where they excite atmospheric gases, causing them to glow. The aurora resembles the same phenomenon that crowns Earth's polar regions. But this Hubble image, taken in ultraviolet light, also shows the glowing "footprints" of three of Jupiter's largest moons: Io, Ganymede, and Europa.

Courtesy of NASA/ESA, John Clarke (University of Michigan)

Jupiter's Magnetosphere
This image taken by the ion and neutral mass spectrometer instrument on NASA's Cassini spacecraft makes the huge magnetosphere surrounding Jupiter visible in a way no instrument on any previous spacecraft has been able to do. The magnetosphere is a bubble of charged particles trapped within the magnetic environment of the planet. A magnetic field is sketched over the image to place the energetic neutral atom emissions in perspective. This sketch extends in the horizontal plane to a width 30 times the radius of Jupiter. Also shown for scale and location are the disk of Jupiter (black circle) and the approximate position (yellow circles) of the doughnut-shaped torus created from material spewed out by volcanoes on Io.

Some of the fast-moving ions within the magnetosphere pick up electrons to become neutral atoms, and once they become neutral, they can escape Jupiter's magnetic field, flying out from the magnetosphere at speeds of thousands of kilometers, or miles, per second.

Jupiter's Auroras
These HST images, reveal changes in Jupiter's auroral emissions and how small auroral spots just outside the emission rings are linked to the planet's volcanic moon, Io. The top panel pinpoints the effects of emissions from Io. The image on the left, shows how Io and Jupiter are linked by an invisible electrical current of charged particles called a flux tube. The particles, ejected from Io by volcanic eruptions, flow along Jupiter's magnetic field lines, which thread through Io, to the planet's north and south magnetic poles.

The top-right image shows Jupiter's auroral emissions at the north and south poles. Just outside these emissions are the auroral spots called "footprints." The spots are created when the particles in Io's "flux tube" reach Jupiter's upper atmosphere and interact with hydrogen gas, making it fluoresce.

The two ultraviolet images at the bottom of the picture show how the auroral emissions change in brightness and structure as Jupiter rotates. These false-color images also reveal how the magnetic field is offset from Jupiter's spin axis by 10 to 15 degrees. In the right image, the north auroral emission is rising over the left limb; the south auroral oval is beginning to set. The image on the left, obtained on a different date, shows a full view of the north aurora, with a strong emission inside the main auroral oval.

Credits: John T. Clarke and Gilda E. Ballester (University of Michigan), John Trauger and Robin Evans (Jet Propulsion Laboratory), and NASA.

The Great Red Spot
This dramatic view of Jupiter's Great Red Spot and its surroundings was obtained by Voyager 1 on Feb. 25, 1979, when the spacecraft was 9.2 million kilometers (5.7 million miles) from Jupiter. Cloud details as small as 160 kilometers (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. (Courtesy NASA)

False Color of Jupiter's Great Red Spot
This image is a false color representation of Jupiter's Great Red Spot taken with Galileo's imaging system through three different near-infrared filters. This is a mosaic of eighteen images (6 in each filter) that were taken over a period of 6 minutes on June 26, 1996. The Great Red Spot appears pink and the surrounding region blue because of the particular color coding used in this representation. The red channel is the reflectance of Jupiter at a wavelength where methane strongly absorbs (889nm). Because of this absorption, only high clouds can reflect sunlight in this wavelength. The green channel is the reflectance in a wavelength where methane absorbs, but less strongly (727nm). Lower clouds can reflect sunlight in this wavelength. Finally, the blue channel is the reflectance in a wavelength where there are essentially no absorbers in the Jovian atmosphere (756nm) and one sees light reflected from the deepest clouds. Thus, the color of a cloud in this image indicates its height, with red or white being highest and blue or black being lowest. This image shows the Great Red Spot to be relatively high, as are some smaller clouds to the northeast and northwest that are surprisingly like towering thunderstorms found on earth. The deepest clouds are in the collar surrounding the Great Red Spot, and also just to the northwest of the high (bright) cloud in the northwest corner of the image. Preliminary modelling shows these cloud heights to range about 50km in altitude. (Courtesy NASA/JPL)

Ring of Jupiter
The ring of Jupiter was discovered by Voyager 1 in March of 1979. This image was taken by Voyager 2 and has been pseudo colored. The Jovian ring is about 6,500 kilometers (4,000 miles) wide and probably less than 10 kilometers (6.2 miles) thick. (Copyright Calvin J. Hamilton)

The Jovian System
The best of the Jupiter system is pictured in this collage of images acquired by the Voyager and Galileo spacecraft. Jupiter is the largest planet in our solar system. The four largest moons of Jupiter are known as the Galilean moons and are named Callisto, Ganymede, Europa, and Io. Inside the orbits of the Galilean moons are Thebe, Amalthea, Adrastea, and Metis. At the lower right is shown the Valhalla region of Callisto. Ganymede is toward the bottom middle. Europa is a little above and to the right of Ganymede. Io is the top, left-most moon. Between Io and Jupiter are four little moons. The top-most little moon is Amalthea. Below and to the right of Amalthea are Metis and Adrastea. To the left of Adrastea is Thebe. (Copyright Calvin J. Hamilton)

Moons of Jupiter
This image shows to scale Jupiter's moons Amalthea, Io, Europa, Ganymede, and Callisto. (Copyright Calvin J. Hamilton)

Rings of Jupiter

Name	Distance*	Width	Thickness	Mass	Albedo
Halo	92,000 km	30,500 km	20,000 km	?	0.05
Main	122,500 km	6,440 km	< 30 km	1 x 10^13 kg	0.05
Inner Gossamer	128,940 km	52,060 km	?	?	0.05
Outer Gossamer	181,000 km	40,000 km	?	?	0.05

*The distance is measured from the planet center to the start of the ring.

Jupiter's Moon Summary

Nearly four centuries ago Galileo Galilei turned his homemade telescope towards the heavens and discovered three points of light, which at first he thought to be stars, hugging the planet Jupiter. These stars were arranged in a straight line with Jupiter. Sparking his interest, Galileo observed the stars and found that they moved the wrong way. Four days later another star appeared. After observing the stars over the next few weeks, Galileo concluded that they were not stars but planetary bodies in orbit around Jupiter. These four stars have come to be know as the Galilean satellites.

Over the course of the following centuries another 12 moons were discovered bringing the total to 16. During the last few years the total number of satellites that have discovered is 62. Provisional designators are given until they are officially confirmed and named. Finally in 1979, the strangeness of these frozen new worlds was brought to light by the Voyager spacecrafts as they swept past the Jovian system. Again in 1996, the exploration of these worlds took a large step forward as the Galileo spacecraft began its long term mission of observing Jupiter and its moons.

Most of Jupiter's moons are relatively small and seem to have been more likely captured than to have been formed in orbit around Jupiter. The four large Galilean moons, Io, Europa, Ganymede and Callisto, are believed to have accreted as part of the process by which Jupiter itself formed. The following table summarizes the radius, mass, distance from the planet center, discoverer and the date of discovery of each of the moons of Jupiter:

Moon	#	Radius (km)	Mass (kg)	Distance (km)	Discoverer	Date
Io	I	1,815	8.94e+22	421,600	Marius-Galileo	1610
Europa	II	1,569	4.80e+22	670,900	Marius-Galileo	1610
Ganymede	III	2,631	1.48e+23	1,070,000	Marius-Galileo	1610
Callisto	IV	2,400	1.08e+23	1,883,000	Marius-Galileo	1610
Amalthea	V	135x84x75	7.17e+18	181,300	E. Barnard	1892
Himalia	VI	93	9.56e+18	11,480,000	C. Perrine	1904
Elara	VII	38	7.77e+17	11,737,000	C. Perrine	1905
Pasiphae	VIII	25	1.91e+17	23,500,000	P. Melotte	1908
Sinope	IX	18	7.77e+16	23,700,000	S. Nicholson	1914
Lysithea	X	18	7.77e+16	11,720,000	S. Nicholson	1938
Carme	XI	20	9.56e+16	22,600,000	S. Nicholson	1938
Ananke	XII	15	3.82e+16	21,200,000	S. Nicholson	1951
Leda	XIII	8	5.68e+15	11,094,000	C. Kowal	1974
Thebe	XIV	55x45	7.77e+17	221,895	S. Synnott	1979
Adrastea	XV	12.5x10x7.5	1.91e+16	128,971	Jewitt-Danielson	1979
Metis	XVI	20	9.56e+16	127,969	S. Synnott	1979
Callirrhoe	XVII	2.4	?	24,296,,000	Spacewatch	1999
S/1975 J1 S/2000 J1		4	?	7,435,000	Sheppard et al	2000
S/2000 J11		2	?	12,654,000	Sheppard et al	2000
S/2000 J10		1.9	?	20,375,000	Sheppard et al	2000
S/2000 J3		2.6	?	20.733,000	Sheppard et al	2000
S/2000 J5		2.2	?	21,019,000	Sheppard et al	2000
S/2000 J7		3.4	?	21,162,000	Sheppard et al	2000
S/2000 J9		2.5	?	21,734,000	Sheppard et al	2000
S/2000 J4		1.6	?	21,948,000	Sheppard et al	2000
S/2000 J6		1.9	?	22,806,000	Sheppard et al	2000
S/2000 J8		2.7	?	23,521,000	Sheppard et al	2000
S/2000 J2		2.6	?	24,164,000	Sheppard et al	2000