Investigating Astronomy Timothy F. Slater, Roger A. Freeman Chapter 7 Observing the Dynamic Giant Planets
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1 Investigating Astronomy Timothy F. Slater, Roger A. Freeman Chapter 7 Observing the Dynamic Giant Planets Observing Jupiter and Saturn The disk of Jupiter at opposition appears about two times larger than the disk of Saturn at opposition, which is about two times farther away. Both planets display dark and light bands, though these are fainter on Saturn. (As viewed from on the Earth) Jupiter and Saturn As viewed from Voyager space probe Jupiter and Saturn The Appearance of Jupiter The Appearance of Saturn Please insert figure 43.1 Jupiter 5 AU from the Sun 11x Earth s diameter 300x Earth s mass Saturn 9.5 AU from the Sun 9.5x Earth s diameter 100x Earth s Mass Parallel bands of clouds Dark belts Light zones 90% H 2, 10% He, traces of methane, ammonia and water Outer atmosphere has a temperature of 160K Rotates once every 9.9 hours Visibly flattened! Parallel bands of clouds Similar to Jupiter s, but not as distinct 96% H 2, 4% He, traces of hydrogen-rich compounds Outer atmosphere has a temperature of 130K Rotates once every 10.7 hours Even flatter than Jupiter! Solid Rotation versus Differential Rotation All parts of a solid object rotate together. A rotating fluid displays differential rotation. The Interiors of the Gas Giants Please insert figure 43.3 The Compositions of Jupiter and Saturn Rocky core An outer core of liquid ices A layer of helium and liquid metallic hydrogen A layer of helium and ordinary molecular hydrogen (H 2 ) Saturn has more rocky core and less liquid
2 On Jupiter, these wind shears give rise to enormous vortices, or storms, seen as white, brown or red ovals in its clouds The Great Red Spot on Jupiter is one such vortex Rises 50 km above surrounding clouds Wind speeds of 500 km/hr! Changes size over time The Great Red Spot The Great Red Spot is a storm that has lasted for at least 300 years! Galileo saw it, and it hasn t changed much It is changing color slowly, however. Jupiter s Atmosphere Jupiter s Bands This visible-light image of Jupiter was made by the Voyager 1 craft. Bright and dark areas in this Earth-based infrared image, taken at the same time, correspond to high and low temperatures, respectively. Jupiter and Saturn s Cloud Layers The black curves show temperature versus altitude in each atmosphere, as well as the probable arrangements of the cloud layers. Beneath both planets cloud layers, the atmosphere is composed almost entirely of hydrogen and helium. (Zero altitude = 1/10 of Earth s atmospheric pressure.) Magnetic Fields The liquid metallic hydrogen in Jupiter and Saturn can carry electrical currents, similar to the liquid core of the Earth fields. These currents generate very large magnetic -Jupiter s is 20,000 times as strong as Earth s, and if it were visible, would appear larger than the full Moon in our sky! -Saturn s field is 500 times as strong as Earth s Both Jupiter and Saturn experience auroras ConceptCheck: Will Jupiter s rocky moons, such as Ganymede, exhibit differential rotation? If Jupiter and Saturn formed with nearly the same chemical composition, why might Jupiter be observed to have more helium than Saturn? Besides color, what is the difference between Jupiter s white ovals and brown ovals? Why might Jupiter s cloud layers be more compressed than Saturn s? The Discovery of Uranus In 1781 a new planet was discovered by W. Herschel Originally thought to be a comet! Herschel named it Georgium Sidus (George s Star) after King George III Name changed to Uranus to stay consistent with the mythological names of the other planets A New Method of Discovery It was noted that Uranus was not following its calculated orbit Another planet must be influencing its orbit Two scientists calculated where the new planet should be Astronomers looked at this location, and found Neptune! Galileo saw Neptune while looking at Jupiter s moons, but didn t realize what it was
3 Neptune is a cold, bluish world with Jupiter-like atmospheric features. Neptune has essentially the same atmospheric composition as Uranus Receives half the energy from the Sun as Uranus Continued contraction fuels Neptune s storms? The Atmospheres of Uranus and Neptune The atmospheres of both Uranus and Neptune are rich in hydrogen and helium Both have larger amounts of methane, giving them their blue color Methane crystals scatter blue light, and methane gas absorbs red light Both planets are very cold Uranus: 80K (-315 F) Neptune: 75K (-324 F) Densities: Uranus: 1.3 kg/liter Neptune: 1.6 kg/liter Uranus s Atmosphere Faint cloud markings became visible in images of Uranus only after extreme computer enhancement. The color is due to methane in the planet s atmosphere, which absorbs red light but reflects green and blue. The substances that make up the clouds on Jupiter and Saturn are not available on Uranus. Like wispy, high-altitude cirrus clouds in the Earth s atmosphere, these clouds are thought to be made of ice crystals. The difference is that Neptune s cirrus clouds are probably methane ice, not water ice. Neptune s Atmosphere Internal Structures of Uranus and Neptune Both Uranus and Neptune have a rocky core, resembling a terrestrial planet a mantle of liquid water with ammonia dissolved in it an outer layer of liquid molecular hydrogen and liquid helium ConceptCheck: If methane were absent from Uranus s atmosphere, what color would it appear? Why would scientists be surprised that Neptune had active belts and zones, unlike Uranus? Uranus s Axial Tilt The magnetic fields of Earth, Jupiter, and Saturn nearly align with their respective rotation axes. Major Moons Uranus is tipped almost 90 degrees to the ecliptic plane Possible that a collision early in its history tipped the axis, and splashed out material for its moons This inclination means that for half of Uranus orbit, one hemisphere is in uninterrupted daylight, and the other hemisphere is in darkness! In contrast, the magnetic and geographic poles of Uranus and Neptune differ greatly. Jupiter has 50 named + 14 provisional moons = 64 Galilean moons, discovered by Galileo, using his new telescope. Quite unusual moons! IO most volcanically active body in solar system EUROPA probably has a subsurface ocean GANYMEDE largest moon in system, larger than Mercury CALLISTO about same size as Mercury, has magnetic field TITAN very dense atmosphere TRITON retrograde motion, coldest object
4 Medium & large moons Enough self-gravity to be spherical Are or were geologically active. Have substantial amounts of ice. Small moons Far more numerous than the medium and large moons. Not enough gravity to be spherical: potatoshaped Satellites in the Outer Solar System Satellites of the giant planets range in size from larger than Mercury to small asteroid-like bodies Some of the satellites are in regular orbits (nearly circular, orbiting in the same direction that the planet spins, and near the planet s equator) Probably formed along with the planets Many of the orbits are irregular, and the satellites appear to be captured bodies Roche s Limit Uranus s has 27 Moons, best known being Miranda Roche limit is the minimum radius at which a satellite (held together by gravitational forces) may orbit without being broken apart by tidal forces. Saturn s rings are inside Saturn s Roche limit, so no moons can form from the particles. All ring particles would form a small moon about the mass of Janus. Miranda appears to have been shattered by an impact Long cracks or faults riddle its surface Huge 20 km cliffs, rolling Hills adjacent to wrinkled terrain The leading hypothesis for Miranda s appearance is that the complex pattern arose as the result of strong tectonic activity that broke the surface into plates Saturn has 53 named Moons, 9 provisional = 62 : Titan may be the most interesting in system Seeing Titan s Surface Titan has a thick atmosphere with a unique chemical composition. The haze surrounding Titan is so dense that little sunlight penetrates to the ground. Titan could have methane rain and lakes of liquid ethane! Visible/ infrared imagery Titan s rocks are chunks of water ice. Riverbeds meandering across the Xanadu highlands of Titan. These are believed to have formed by the flow of liquid methane and ethane.
5 Lakes on Titan: Possibly liquid hydrocarbons (ethane, methane) Neptune has 13 known Moons: Triton is one of the most unusual only major moon to orbit in a CW (retrograde) orbit A conspicuous absence of large craters Triton has a young surface on which the scars of ancient impacts have largely been erased by tectonic activity. Areas that resemble frozen lakes and may be the calderas of extinct ice volcanoes. A dimpled, wrinkled terrain that resembles the skin of a cantaloupe. TRITON Volcanically active (Nitrogen & methane) Triton currently has the record as the coldest body in solar system F (27 K above absolute zero) Colder than Pluto ConceptCheck: All of the Gas Giants Have Ring Systems Rings of Jupiter - Voyager back view and Galileo detailed image Prior to the Huygens probe, why was so little known about the surface of Titan? How was an atmosphere detected on Triton? Uranus Neptune Computer Enhanced false color image of Saturn s ring system Uranus has a system of 13 thin rings
6 The rings are NOT visible from earth or from earth orbit. The dim ring structure of Neptune was imaged by the Voyager spacecraft by blocking out the light from the central planet. Saturn s System of Rings Saturn is visible through the rings, which shows that the rings are not solid. The C ring is so faint that it is almost invisible in this view. Shepherd Satellites The Changing Views of Saturn s Rings Color Variations in Saturn s Rings A close examination of Saturn s rings shows that they are composed of tiny ringlets The thin rings of the gas giants are maintained by shepherd satellites The gravitational pull of these small moons keeps ring particles in line! Saturn s rings are tilted 27 from Saturn s orbital plane. As Saturn orbits, observers on Earth see the rings at various angles. The rings seem to disappear when viewed edge-on. Cassini images show the rings in natural color. Color variations are indicative of slight differences in chemical composition among particles in different parts of the rings. Earth based observations of Uranus rings Now we finally leave the confines of our planetary homes and venture out farther into the realm of the Sun
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