The last two Gas Planets, Uranus and Neptune, are less than half the diameter of Jupiter and Saturn. Both appear a near-sky blue in colored versions constructed from Voyager 2 images. Uranus has five large satellites (and 17 small ones) and Neptune two, plus 6 small ones discovered by Voyager. Both have ring systems, so that all four Giant Planets possess this feature. On this page all of the five large uranian satellites, each with an outer shell of ice, are pictured.
From Saturn, Voyager 2 moved onward,
to pass Uranus and Neptune. As with Saturn, we suggest you take a quick look at the U. of Arizona LPL summaries (by Bill Arnett) of Uranus and Neptune.
As we noted before, both of these outer Giants are
about 40% the diameter of Jupiter. Uranus and Neptune have densities of 1.28
and 1.63 g/cm3, respectively. Both have thick cores composed of rock
mixed with water, ammonia, and methane ices, lack metallic hydrogen mantles,
have thick gaseous envelopes (about 15% of the planet's mass) consisting of
about 83% H, 15% He, 2% CH4 (methane) and traces of other gases.
They also have rather faint, thin rings, and strong but distorted magnetic fields.
Uranus has 22 known satellites, of which 5 are greater than 450 km (280 mi)
in diameter. (Interestingly, many of the satellites discovered by Voyager 2 are named after well-known Shakespearean characters from his plays.) Neptune has 8, of which 2 are greater than 400 km (249 mi) wide.
In this discussion, we describe only the larger ones. Seen in color by Voyager cameras,
both planets appear similar, as shown here (Uranus on left; Neptune right):
Each has a notably bluish color, because methane gas absorbs longer wavelengths (reds and yellows) and reflects shorter wavelengths (blues). The atmospheres possess weak banding and Neptune displays a large Dark Spot and fast moving cloud spots that represent rising plumes and turbulence. Neptune's zonal winds can move as fast as 900 km/hr–the fastest measured, so far, in the solar system. Neptune's Great Dark Spot, shown in detail below, is accompanied by an elongated bright patch (nicknamed "Scooter"). It is evidence of a storm at the time of the Voyager pass. In the late '90s, observations by the Hubble Space Telescope revealed the Spot to be gone (unlike the Great Red Spot on Jupiter).
19-68: Why are Uranus and Neptune different in color from Jupiter and Saturn? ANSWER
Neptune takes 165 years to fully orbit the Sun. Its axis is tilted 29° from the ecliptic. For this reason, like Earth, scientists postulated seasonal changes in the weather patterns exhibited by the bands. If these seasons are analogous to the four on Earth, about 41 years is needed to complete a neptunian season. After 7 years of observations by HST, these changes - brightening and broadening of the bands first noted - seem to confirm that such changes are happening.
Both Uranus and Neptune have a few rings, which
are faint and thin. A ground-based telescope image made by a European Space Agency telescope seems to indicate Uranus' rings are as well-developed as Saturn's.
The rings are actually much more tenuous than those of Saturn. This enhanced Hubble Space Telescope of Uranus highlights both the variations within the atmosphere and its most prominent ring. Note too that this image shows the planet in its proper orientaton, with its rotation axis "flipped" about 90 ° so that it is almost in the plane of the ecliptic along which it orbits.
All told, Uranus has 11 rings, with the outermost (Epsilon) being
much brighter than the others, as shown above. Two small satellites are visible
on either side of the Epsilon ring.
Scientists call these satellites, "shepherds,"
because they seem responsible for keeping that ring intact, by pushing stray
particles back into line and possibly gathering and inserting particles from
beyond. One of the rings around Neptune has a distinctive "braided"
(twisted) structure: The five outermost uranian moons
are also that planet's largest. They occur in this sequence (from the left): Miranda (472 km
[293 mi] in diameter), Ariel (1,158 km [720 mi] in diameter), Umbriel (1,172
km [728 mi] in diameter), Titania (1,580 km [982 mi]in diameter), and Oberon
(1,524 km [947 mi] in diameter). Oberon is the farthest from Uranus at 583,300
km (362,463 mi). Each has an icy surface, extending to unknown depths, making
up about 40-50% of the volume but ending in a rocky interior. The last four comprise a group, in
which all show strong similarities, with their dominant features being craters
(especially Umbriel and Oberon) and deep (some greater than 10 km [6.2 mi]),
interconnected, gash-like valleys (particularly Titania and Ariel.
One hypothesis for the origin of
these cracks contends that the satellites once had enough internal heat to melt
the exteriors into liquid water, which induced tensional fracturing, when it
later froze and expanded the ice. 19-69:
Which of the four above satellites appears to be older? ANSWER
Miranda is unique among the uranian
satellites but, excepting its much smaller size, strongly resembles Ganymede
in the Jovian group. By serendipity, Voyager 2 made the closest approach to
Miranda of any of the satellites, so it could image the peculiar terrains in
detail. Investigators based this flyby decision on the need to use this satellite
to give the spacecraft a gravitational boost towards Neptune. First, look at
the full view (left), a mosaic of one face. Then (right), view a close-up
of the surface. Still another close view of the mirandan
surface shows high fault scarps and grabens in jumbled
terrains. Most of the ten small satellites discovered by Voyager (six more have since been found in photographic plates exposed through Earth-based telescopes) were not sharply imaged. An exception is Puck, about a 200 km diameter object, shown below. At least some of these bodies are probably captured asteroids.
Two sharply contrasting terrains
are evident. Much of Miranda's surface consists of rather bright, heavily
cratered terrains, similar to the above four satellite exteriors. But there
are three large oval-to-rectangular terrains (called coronae), whose physiographies
are quite different (to each other and to the dominant terrain). They may
contain subparallel grooves, several as deep as 2 km (1.2 mi), or alternating
light-dark bands, or ridges and stripes that take sharp bends. A closer view
(at bottom, above) of ridged terrain shows the generally abrupt boundaries
of these terrains with the encompassing older terrain. Scientists still debate
the origin of these patches. An early interpretation considered them to be
fragments of a shattered proto-Miranda or some other disrupted satellite,
incorporated in a re-assembling satellite. The paucity of craters in these
isolated terrains argues against this. Another opinion holds them to be a
mix of rock and ice that formed a crust, which broke up and was invaded by
upwelled ice masses from the interior.
19-70: Develop
an argument against the impact disruption hypothesis. ANSWER
Primary Author: Nicholas M.
Short, Sr. email: nmshort@ptd.net