1 (2 G) Jupiter and Earth to scale. Jupiter is 11x diameter of Earth and over 1400x volume. One day on Jupiter lasts less than 10 hours

2 (2 J) The giant planet from 33x10⁶ km distance; the resolution is about 600 km

3 (3 J) Jupiter with Io and Europa in front at a distance of 20x10⁶ km

4 (4 J) The red spot comes in to view. The spot is in the southern hemisphere, turning anticlockwise. North of the red spot lies a curious darker section of the South Equatorial Belt. To the lower left of the red spot lies one of 3 long-lived white ovals

5 (5 J) The red spot in detail, 3 months after the previous picture was taken. Detail has changed significantly; for example a different white oval cloud is seen to the South of the red spot

6 (8 J) The neighbourhood of the red spot, extending from equator to near Southern polar latitudes near the spot. Cloud vortices can be seen forming out of the wave structures

7 (9 J) The rings of Jupiter, first seen by Voyager 1 in March 1979. The estimated thickness is less than 30 km

8 (10 G) The impact of comet Shoemaker-Levy 9 on Jupiter in 1994 was recorded by the Galileo probe at a distance of 238x10⁶ km. In the 2nd, 3rd and 4th images covering only 7 seconds, a point of light appears, brightens and fades

9 (10 J) The Galilean satellites, shown to scale. (I Eat Green Carrots). All are large and fairly close to Jupiter. Io is larger than the Moon, Ganymede larger than Mercury.. There are 4 small moons even closer, with tiny Amalthea circling every 12 hours just 1.5 radii away from the cloud tops. There are many other moons further away

10 (14 G) 3 full disk colour views of Io, the most volcanic body in the solar system. A comparison with the Voyager pictures taken 17 years previously show a dozen substantial areas have been re-surfaced by volcanic activity. Red and black areas are the most recent; much of the surface is yellow or light greenish

11 (15 G) Io in front of Jupiter (Sept. 1996) centred on the side that always faces away from Jupiter. Io’s surface changes sufficiently quickly to detect differences that took place in the summer of 1996.

12 (13 G) Eruption on Io, throwing out a plume extending about 100 km into space. The plume is thought to be largely SO₂ and sulphur vapour, which condenses as it rises. The RH images show Voyager (1979) image at top and Galileo (1996) image below of volcano Ra Patera

13 (16 G) Changing volcanoes on Io. The left-hand image was taken of an active volcano (Prometheus) in 1979. In 1996 it is still showing an active plume though from a different location and new surface lave flows are present.

14 (23 G) Io glowing in the dark (LHS). Volcanic hot spots over 700K and aurora glowing green. The B&W picture is voyager’s daylight image of the same part of the moon

15 (17 G) Ice covered Europa. The LH image is approximately natural colour, the RH has false colour in blue to enhance the difference between coarse-grained ice (dark) and fine-grained ice (light blue). The dark brown patches are rocky areas; long lines are huge fractures, larger ones over 1000 km long

16 (16 J) Europa close up showing the fractures that give it the appearance of a cracked billiard ball. It is the brightest of the Galilean satellites and it has been speculated that its crust of ice is perhaps 100 km thick

17 (21 G) A complex of ridges over an area 238 x 225 km. Ridges seem to show areas where surface has been split apart and partly filled in by material coming from below. The small no. of impact craters point to a young surface.

18 (18 G) Impact craters on Europa look different from those on the Earth’s Moon because Europa’s surface is largely water ice. This image covers an area of 48 x 91 km

19 (19 G) Tiny area of Europa, 9.6 x 16 km. The smallest visible feature is about the size of a football pitch

20 (19 J) Distant Ganymede seen by Voyager 2. Notice the light, bluish regions near the poles - water ice or frost?

21 (18 J) Ganymede closer up, seen near the terminator. Another icy world with bright rayed craters, suggesting that impact has revealed subsurface ice.

22 (25 G) Fine detail on Ganymede, illustrated by Galileo images at 74 m per pixel superposed on the best Voyager image at 1.3 km per pixel. Parallel ridges and troughs are the principal features of the bright regions of Ganymede

23 (26 G) New terrain overlaying old terrain overlaying even older terrain. Ganymede is tectonically active, as can be seen in this picture of an area 54 x 90 km. The small craters are secondary ejecta from a distant larger crater

24 (28 G) Image 55 x 35 km showing detail on one of the bright regions that make up about half of Ganymede’s surface. Pock-marked, ancient heavily cratered terrain at the top is cut by younger terrain with lines of ridges in lower left, and a large impact crater. Ridged regions show extension and shear.

25 (29 G) Area of ancient impact craters on Ganymede’s crust of dirty water ice. This area (46 x 64 km) is probably billions of years old. At the left is half a crater 19 km in diameter

26 (31 G) Ice frosted crater tops on Ganymede in an image 18 x 18 km. The North face walls are encrusted in ice.

27 (32 G) Image processed stereo view of Galileo Regio of Ganymede showing typical deep furrows and smaller impact craters

28 (12 J) Callisto seen by Voyager, with some false colour to enhance surface contrast. The surface has crater densities resembling those on the Moon and Mercury.

29 (13 J) Valhalla impact crater on Callisto - the largest visible impact crater in the solar system. It is very ancient. The bright central area is about 300 km across and the discontinuous concentric ridges extend out some 1500 km form the centre

30 (34 G) central zone about 11 km across of Valhalla, showing detail as small as 60 m across. The smaller craters have been softened by downward movement of debris that reveal bright, ice-rich surfaces. Very small craters seem to have been obliterated.

31 (33 G) Asgard impact structure on Callisto approximately 1700 km across. The rings are scarps near the central zone and troughs in the outer margins

32 (35 G) A chain of impact craters on Callisto believed to result from a succession of impacts, like that of the comet Shoemaker-Levy 9. The area covered is about 8 km across and the smallest visible crater only 130 m in diameter. Bright areas are where downslope movement has exposed subsurface ice. There is a shortage of small craters compared with the number expected, indicating some surface changes on a small scale over hundreds of millions of years. Overall, Callisto shows the heavily cratered surface expected of an old body

34 (1) HST view of Saturn from a distance of 1.4x10⁹ km, superior to any taken from Earth. The Cassini division of the rings is clearly seen

35 (2) Storm on Saturn, appearing as a white arrowhead near the equator. The white clouds are ammonia-ice crystals. Major storms seem to follow a cycle of two Saturnian years (57 Earth years), when it’s summer in the Northern hemisphere on Saturn

36 (3) Voyager 2 approaches. 3 of Saturn’s icy moons are seen - Tethys (1050 km diam.), shadowed on the S. hemisphere of Saturn, Dione (1120 km diam.) and Rhea (1530 km diam.). The shadow of small Mimas can be seen above that of Tethys. The pastel colours of Saturn revel weather structures

37 (4) Voyager 1 view, showing cloud belts more clearly than can be seen from Earth

38 (6) Cyclones, spots and jet streams in Saturn's atmosphere, with emphasis in false colour. Note the 3 spots. The Westernmost shows anti-cyclonic rotation and is about 3000 km across

39 (7) Atmospheric features on Saturn. The temperatures are lower on Saturn than on Jupiter and gravity weaker, producing blander atmospheric features.

40 (9) Rotation of the spokes, not yet adequately explained. Saturn’s magnetic field appears to be responsible for the spokes

41 (10) Detail in the rings. All the Jovian planets have rings but Saturn’s are in a class of their own. The Voyager probe showed the amazing detail seen here

42 (12) Closer detail of the rings. The colour differences have been enhanced to try to pinpoint differences in chemical composition of the rocks in the rings. Even here, the rings are 8.9x10⁶ km away

43 (13) The C ring in false colour showing more than 60 bright and dark ringlets. The material is generally bland and grey, the colour of dirty ice

44 (17) Titan's atmospheric bands. The extended haze is composed of sub-micron sized particles and prevents anything but the haziest view of surface features

45 (18) The surface of Titan, as seen by Hubble in the best view yet. The resolution is about 500 km; the prominent bright area about 4000 km across

46 (19) Enceladus, whose surface is a bit like Ganymede’s, though Enceladus is only one tenth the size. You can see sets of groves 10s of km long and significant areas of young uncratered surface

47 (21) Dione close up showing many impact craters, the largest 100 km across with a well-developed central peak. Sinuous valleys break the icy crust

48 (22) A huge crater on Mimas, more than 100 km across with a central peak, with small craters in abundance

49 (23) Close up of Hyperion. This moon is an irregular disc shape with longest dimension 360 km

51 (2) Uranus in true colour and false colour. On the left is the view from 9.1x10⁶ km as the eye would see it, the dark shadings on the upper right is the terminator; on the right, colour enhancement shows the darker polar hood.

52 (8) The major rings, with a newly discovered (by this picture in Jan 1986) 10th ring near the top. This ring orbits at a radius of 50,000 km. The picture resolution of 10 km fails to resolve detail in most rings.

53 (10) 2 shepherd satellites have an important role in preventing rings from spreading out, adding a dynamical stability. This was the first picture showing 9 rings in reflected sunlight

54 (1) Rocky Miranda and gaseous Uranus, a montage of Voyager 2 pictures with the artists addition of the rings

55 (11) Oberon, Uranus’ outermost moon showing clearly impact craters with bright rays on the icy surface, reminiscent of Callisto. A large mountain about 6 km high is visible on the lower left

56 (13) Titania, showing abundant impact craters on this ancient pockmarked surface and prominent fault valleys scratching across Titania. The longest are up to 1500 km long and 75 km wide; the largest impact craters well over 100 km across

57 (14) Umbriel, showing heavy cratering on this darkest of Uranus large moons. It’s Albedo is similar to Lunar highland areas

58 (15) Ariel, much of whose surface is densely pitted with craters only just visible at the limit of resolution of this picture (2.5 km). Numerous valleys and fault scarps criss-cross the terrain, showing where blocks of land have dropped down and, in places, been partly filled with deposits. Sinuous valleys in younger material might have been formed by the flow of fluids.

59 (17) Miranda at 480 km in diameter is the smallest of the major moons. It is very heavily faulted with sets of parallel fault valleys and ridges. First of 4 slides of Miranda

60 (18) Complex terrain on Miranda, showing a dramatically varied surface at a resolution of about 800 m. On the right is rugged, older, more cratered, higher terrain that is adjacent to lower, striated land

61 (19) 20 km high cliffs on Miranda visible on these even closer view. Ridges and valleys were probably produced by compression of the plate tectonics

62 (20) Canyons and craters on Miranda in another close-up showing a bewildering variety of fractures, grooves and craters as well as features of different albedos. The variety of features indicate a long and complex geological evolution

64 (2) Neptune, showing 2 of the 4 cloud features tracked by Voyager 2 in 1989. The prominent dark oval near the western limb at 12° S circulate the large planet every 18.3 hrs; the associated bright clouds change their appearance in as little as 4 hours. The second dark spot is at 54° S, near the terminator

65 (5) Limb haze on Neptune in this false colour picture that shows deep objects in blue and higher altitude objects in white. The light, bright feature is a high altitude methane cloud just south of the great dark spot

66 (6) Neptune from 5 million km. 3 prominent features at different latitudes all move eastward at different rates and are not often in the same frame. This picture was made at a time predicted by a weather forecast made 8 days earlier, which was pretty accurate

67 (7) Great dark spot and scooter. The scooter is the middle feature that moves East blown by winds at up to 400 mph

68 (11) Haze and other features on Neptune in this false colour image. Those that appear red are where sunlight has been scattered before passing through large quantities of methane that give Neptune its blue colouring

69 (16) The 2 main rings of Neptune, about 53,000 km and 63,000 km from the planet. The rings are more broken and clumpy than most planetary rings and the change of reflectivity with angle of view suggests they are made of finer dust particles than most of Uranus’ and Saturn’s rings

70 (14) 2 rings and 2 shepherding moons that give the rings stability

71 (20) Looking back at Neptune and Triton as Voyager 2 heads out of the solar system at an angle of 48° to the ecliptic. [The green worm is a reproduction mark!]

72 (2) Triton from 530,000 km with a resolution of 10 km. The S. pole is bottom left and in continuous sunlight at the season shown. No large impact craters are visible, suggesting that the surface has been renewed within the past billion years. Triton has different terrains in different parts

73 (3) Icy ridges on Triton’s northern hemisphere

74 (4) Flooded basins on Triton, the large one being 200 km by 400 km. These are interpreted as large impact craters modified and filled with ice. Notice the small number of impact craters

75 (7) Triton from 40,000 km showing detail as small as 750 m. This terrain of regular, roughly circular depressions separated by rugged ridges is like nothing else seen in the solar system. The depressions are probably not impact craters (they are too similar to each other and regularly spaced) but represent local melting and collapse of an icy crust

76 (8) Varied terrain on Triton shown on this cylindrical false-colour terrain map

77 (11) So called lava Basins, representing an eruption of ice lavas of low viscosity. [A mixture of ices - water, carbon dioxide, ammonia, methane?]

78 (12) Oblique view of a caldera-like depression regions on Triton, computer generated from aerial survey data. Topographic features rise to about 1 km high around the 13 km crater shown

79 (18) 3 new moons about Neptune. The inner 2 orbit Neptune in only just over 7 hours

80 (20) Moon 1989 N1 from 146,000 km. Another new moon discovered in 1989 with an average radius of 200 km and travelling fast. It is dark (albedo 6%) and grey, showing hints of catering