7.1 Exploring the Outer Planets
The giant planets hold most of the mass in our planetary system. Jupiter alone exceeds the mass of all the other planets combined (Figure 7.1). The material available to build these planets can be divided into three classes by what they are made of: “gases,” “ices,” and “rocks” (see Table 7.1). The “gases” are primarily hydrogen and helium, the most abundant elements in the universe. The way it is used here, the term “ices” refers to composition only and not whether a substance is actually in a solid state. “Ices” means compounds that form from the next most abundant elements: oxygen, carbon, and nitrogen. Common ices are water, methane, and ammonia, but ices may also include carbon monoxide, carbon dioxide, and others. “Rocks” are even less abundant than ices, and include everything else: magnesium, silicon, iron, and so on.
Jupiter
PIA02873: High Resolution Globe of Jupiter by NASA/JPL/University of Arizona, NASA Media Licence.
| Type of Material | Name | Approximate % (by Mass) |
|---|---|---|
| Gas | Hydrogen (H2) | 75 |
| Gas | Helium (He) | 24 |
| Ice | Water (H2O) | 0.6 |
| Ice | Methane (CH4) | 0.4 |
| Ice | Ammonia (NH3) | 0.1 |
| Rock | Magnesium (Mg), iron (Fe), silicon (Si) | 0.3 |
In the outer solar system, gases dominate the two largest planets, Jupiter and Saturn, hence their nickname “gas giants.” Uranus and Neptune are sometimes called “ice giants” because their interiors contain far more of the “ice” component than their larger cousins. The chemistry for all four giant planet atmospheres is dominated by hydrogen. This hydrogen caused the chemistry of the outer solar system to become reducing, meaning that other elements tend to combine with hydrogen first. In the early solar system, most of the oxygen combined with hydrogen to make H2O and was thus unavailable to form the kinds of oxidized compounds with other elements that are more familiar to us in the inner solar system (such as CO2). As a result, the compounds detected in the atmosphere of the giant planets are mostly hydrogen-based gases such as methane (CH4) and ammonia (NH3), or more complex hydrocarbons (combinations of hydrogen and carbon) such as ethane (C2H6) and acetylene (C2H2).
Exploration of the Outer Solar System So Far
Eight spacecraft, seven from the United States and one from Europe, have penetrated beyond the asteroid belt into the realm of the giants. Table 7.2 summarizes the spacecraft missions to the outer solar system.
| Planet | Spacecraft1 | Encounter Date | Type |
|---|---|---|---|
| Jupiter | Pioneer 10 | December 1973 | Flyby |
| Pioneer 11 | December 1974 | Flyby | |
| Voyager 1 | March 1979 | Flyby | |
| Voyager 2 | July 1979 | Flyby | |
| Ulysses | February 1992 | Flyby during gravity assist | |
| Galileo | December 1995 | Orbiter and probe | |
| Cassini | December 2002 | Flyby | |
| New Horizons | February 2007 | Flyby during gravity assist | |
| Juno | July 2016 | Orbiter | |
| Saturn | Pioneer 11 | September 1979 | Flyby |
| Voyager 1 | November 1980 | Flyby | |
| Voyager 2 | August 1981 | Flyby | |
| Cassini | July 2004 | Orbiter | |
| Uranus | Voyager 2 | January 1986 | Flyby |
| Neptune | Voyager 2 | August 1989 | Flyby |
The first spacecraft to investigate the regions past Mars were the NASA Pioneers 10 and 11, launched in 1972 and 1973 as pathfinders to Jupiter. One of their main objectives was simply to determine whether a spacecraft could actually navigate through the belt of asteroids that lies beyond Mars without getting destroyed by collisions with asteroidal dust. Another objective was to measure the radiation hazards in the magnetosphere (or zone of magnetic influence) of Jupiter. Both spacecraft passed through the asteroid belt without incident, but the energetic particles in Jupiter’s magnetic field nearly wiped out their electronics, providing information necessary for the safe design of subsequent missions.
Pioneer 10 flew past Jupiter in 1973, after which it sped outward toward the limits of the solar system. Pioneer 11 undertook a more ambitious program, using the gravity of Jupiter to aim for Saturn, which it reached in 1979. The twin Voyager spacecraft launched the next wave of outer planet exploration in 1977. Voyagers 1 and 2 each carried 11 scientific instruments, including cameras and spectrometres, as well as devices to measure the characteristics of planetary magnetospheres. Since they kept going outward after their planetary encounters, these are now the most distant spacecraft ever launched by humanity.
Voyager 1 reached Jupiter in 1979 and used a gravity assist from that planet to take it on to Saturn in 1980. Voyager 2 arrived at Jupiter four months later, but then followed a different path to visit all the outer planets, reaching Saturn in 1981, Uranus in 1986, and Neptune in 1989. This trajectory was made possible by the approximate alignment of the four giant planets on the same side of the Sun. About once every 175 years, these planets are in such a position, and it allows a single spacecraft to visit them all by using gravity-assisted flybys to adjust course for each subsequent encounter; such a maneuver has been nicknamed a “Grand Tour” by astronomers.
The Jet Propulsion Laboratory has a nice video called Voyager: The Grand Tour that describes the Voyager mission and what it found.
Engineering and Space Science: Teaching an Old Spacecraft New Tricks
By the time Voyager 2 arrived at Neptune in 1989, 12 years after its launch, the spacecraft was beginning to show signs of old age. The arm on which the camera and other instruments were located was “arthritic”: it could no longer move easily in all directions. The communications system was “hard of hearing”: part of its radio receiver had stopped working. The “brains” had significant “memory loss”: some of the onboard computer memory had failed. And the whole spacecraft was beginning to run out of energy: its generators had begun showing serious signs of wear.
To make things even more of a challenge, Voyager’s mission at Neptune was in many ways the most difficult of all four flybys. For example, since sunlight at Neptune is 900 times weaker than at Earth, the onboard camera had to take much longer exposures in this light-starved environment. This was a nontrivial requirement, given that the spacecraft was hurtling by Neptune at ten times the speed of a rifle bullet.
The solution was to swivel the camera backward at exactly the rate that would compensate for the forward motion of the spacecraft. Engineers had to preprogram the ship’s computer to execute an incredibly complex series of maneuvers for each image. The beautiful Voyager images of Neptune are a testament to the ingenuity of spacecraft engineers.
The sheer distance of the craft from its controllers on Earth was yet another challenge. Voyager 2 received instructions and sent back its data via on-board radio transmitter. The distance from Earth to Neptune is about 4.8 billion kilometres. Over this vast distance, the power that reached us from Voyager 2 at Neptune was approximately 10–16 watts, or 20 billion times less power than it takes to operate a digital watch. Thirty-eight different antennas on four continents were used by NASA to collect the faint signals from the spacecraft and decode the precious information about Neptune that they contained.
Enter the Orbiters: Galileo, Cassini, and Juno
The Pioneer and Voyager missions were flybys of the giant planets: they each produced only quick looks before the spacecraft sped onward. For more detailed studies of these worlds, we require spacecraft that can go into orbit around a planet. For Jupiter and Saturn, these orbiters were the Galileo, Cassini, and Juno spacecraft. To date, no orbiter missions have been started for Uranus and Neptune, although planetary scientists have expressed keen interest.
The Galileo spacecraft was launched toward Jupiter in 1989 and arrived in 1995. Galileo began its investigations by deploying an entry probe into Jupiter, for the first direct studies of the planet’s outer atmospheric layers.
The probe plunged at a shallow angle into Jupiter’s atmosphere, travelling at a speed of 50 kilometres per second—that’s fast enough to fly from New York to San Francisco in 100 seconds! This was the highest speed at which any probe has so far entered the atmosphere of a planet, and it put great demands on the heat shield protecting it. The high entry speed was a result of acceleration by the strong gravitational attraction of Jupiter.
Atmospheric friction slowed the probe within 2 minutes, producing temperatures at the front of its heat shield as high as 15,000 °C. As the probe’s speed dropped to 2500 kilometres per hour, the remains of the glowing heat shield were jettisoned, and a parachute was deployed to lower the instrumented probe spacecraft more gently into the atmosphere (Figure 7.2). The data from the probe instruments were relayed to Earth via the main Galileo spacecraft.
Galileo Probe Falling into Jupiter and Juno Image of Jupiter’s South Pole
(a): Galileo probe – artistic impression by NASA/Ames Research Center/C. Kallas, NASA Media Licence.
(b): PIA21382: Jovian Stormy Weather by Enhanced image by John Landino (CC-BY) based on images provided courtesy of NASA/JPL-Caltech/SwRI/MSSS., NASA Media Licence.
The probe continued to operate for an hour, descending 200 kilometres into the atmosphere. A few minutes later the polyester parachute melted, and within a few hours the main aluminum and titanium structure of the probe vaporized to become a part of Jupiter itself. About 2 hours after receipt of the final probe data, the main spacecraft fired its retro-rockets so it could be captured into orbit around the planet, where its primary objectives were to study Jupiter’s large and often puzzling moons.
The Cassini mission to Saturn, a cooperative venture between NASA and the European Space Agency, was similar to Galileo in its two-fold approach. Launched in 1997, Cassini arrived in 2004 and went into orbit around Saturn, beginning extensive studies of its rings and moons, as well as the planet itself. In January 2005, Cassini deployed an entry probe into the atmosphere of Saturn’s large moon, Titan, where it successfully landed on the surface.
The Voyager and Galileo missions to Jupiter were primarily designed to study the moons and the atmosphere of the planet. The next NASA mission, an orbiter called Juno, arrived at Jupiter in July 2016. In order to meet its objectives of studying the jovian magnetosphere, it has a very elongated (eccentric) 55-day orbit, that takes it from 4 thousand kilometres above the cloud tops out to 76 thousand kilometres. The orbit takes the craft over Jupiter’s poles, giving us remarkable close-ups of the polar regions (previous spacecraft viewed the planet from lower latitudes).
Juno was originally designed without a camera, but fortunately scientists rectified this omission, adding a simple downward-looking colour camera to use during close passes by Jupiter. Recognizing the value of such images, both scientific and artistic, it was decided to post the raw images and encourage “citizen scientists” to process them. The product has been many dramatic, brightly coloured views of Jupiter, such as Figure 7.3.
Earth as Seen from Saturn
The Day the Earth Smiled by NASA/JPL-Caltech/Space Science Institute, NASA JPL Media Licence.
Footnotes
1. Both the Ulysses and the New Horizons spacecraft (designed to study the Sun and Pluto, respectively) flew past Jupiter for a gravity boost (gaining energy by “stealing” a little bit from the giant planet’s rotation)
Attribution
“11.1 Exploring the Outer Planets” from Astronomy 2e by Andrew Fraknoi, David Morrison, Sidney C. Wolff, © OpenStax – Rice University is licensed under a Creative Commons Attribution 4.0 International License, except where otherwise noted.
