The Outer Planets.

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Presentation transcript:

The Outer Planets

Introduction Beyond the orbit of Mars, the low temperatures of the solar nebula allowed condensing bodies there to capture hydrogen and hydrogen-rich gases This together with the vast amount of material in the outer Solar System lead to the creation of the four large Jovian planets – Jupiter, Saturn, Uranus, and Neptune Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock Pluto is an exception to these rules resembling the ice and rock makeup of the giant planets’ larger moons The Outer Planets

Jupiter Jupiter’s appearance and physical properties Jupiter is the largest planet both in diameter and mass more than10x Earth’s diameter and 300x the mass Dense, richly colored parallel cloud bands cloak the planet Atmosphere is mainly H, He, CH4, NH3, and H2O Clouds appear to be particles of water, ice, and ammonia compounds Bright colors of clouds may come from complex organic molecules with composition still unknown Figure 9.1 The Outer Planets

Jupiter Jupiter’s interior Interior becomes increasingly more dense as center is approached with its gaseous upper layers turning to liquid hydrogen about 10,000 km below the surface Deeper still, liquid hydrogen compresses into liquid metallic hydrogen, a material scientists only recently created in tiny high-pressure chambers An iron rocky core, a few times bigger than the Earth, probably resides at the center Figure 9.2 The Outer Planets

Jupiter Jupiter’s interior (continued) Jupiter’s atmosphere Jupiter, with a core temperature of about 30,000 K, emits more energy than it receives Possibly due to heat left over from its creation Planet may still be shrinking in size converting gravitational energy into heat Jupiter’s atmosphere General convection pattern: Heat within Jupiter carries gas to the top of the atmosphere High altitude gas radiates into space, cools and sinks Figure 9.3, Figure 9.4 The Outer Planets

Jupiter Jupiter’s ring Jupiter’s moons Jupiter has a thin ring made of tiny particles of rock dust and held in orbit by Jupiter’s gravity Jupiter’s moons Jupiter currently has 63 natural satellites or moons Most of the moons are too small to be seen from Earth and were discovered by examining pictures taken by the Voyager spacecraft Figure 9.6 The Outer Planets

The Outer Planets

Jupiter Jupiter’s moon (continued) Galilean satellites Io, Europa, Ganymede, and Callisto Discovered by Galileo Except for Europa, all are larger than the Moon Ganymede is the largest Moon in the Solar System Figure 9.7, Figure 9.8 The Outer Planets

The Outer Planets

Jupiter Jupiter’s moons (continued) Other observations Galilean average densities indicate their interiors to be composed mainly of rocky material Rest of Jupiter’s moons are much smaller than the Galilean satellites and they are cratered Outermost moons have orbits with high inclinations suggesting that they are captured asteroids The Outer Planets

Saturn Saturn’s Appearance and Physical Properties Saturn is the second largest planet with a diameter and mass more than10x Earth’s diameter and 95x the mass It has a low density which suggests a composition mostly of hydrogen and its compounds Internal structures similar to Jupiter Saturn’s atmosphere looks different than Jupiter’s because Saturn is cold enough for ammonia gas to freeze into cloud particles that veil its atmosphere’s deeper layers Figure 9.10, Figure 9.11 The Outer Planets

Saturn Saturn’s Rings Rings are wide but thin Main band extends from about 30,000 km above its atmosphere to about twice Saturn’s radius (136,000 km) Faint rings can be seen closer to Saturn as well as farther away Thickness of rings: a few hundred meters Rings not solid, but made of a swarm of individual bodies Sizes range from centimeters to meters Composition mainly water, ice, and carbon compounds and is not uniform across rings Figure 9.12, Figure 9.13 The Outer Planets

Saturn Origin of Planetary Rings Rings once thought to be left over remains from a planet’s formation Ring lifetime is short, so for rings to persist they must be replenished Figure 9.14 Animation: Roche breakup of a moon The Outer Planets

The Outer Planets

Saturn Saturn’s Moons Saturn has several large moons and many more smaller ones Like Jupiter, most of the moons form a mini-solar system, but unlike Jupiter, Saturn’s moons are of similar densities indicating that they were not heated by Saturn as they formed Saturn’s moons have a smaller density than those of Jupiter indicating interiors must be mostly ice Most moons are inundated with craters, many of which are surrounded by white markings of shattered ice Figure 9.15, Figure 9.16 The Outer Planets

Saturn Saturn’s Moons (continued) Titan The largest moon, is bigger than Mercury and second to Ganymede in Moon sizes Distance from Sun allows Titan to have a nitrogen atmosphere Clouds shroud surface, which is believed to have oceans of methane Methane rain may fall from clouds The Outer Planets

The Outer Planets

Uranus Introduction Uranus’s Atmosphere Unknown to the ancients, even though visible to the naked eye, Uranus was not discovered until 1781 by Sir William Herschel While small relative to Jupiter/Saturn, Uranus is 4x larger in diameter than Earth and has 15x the mass At its far distance, Uranus is difficult to study from Earth, but even close up images from Voyager reveal a rather featureless object Uranus’s Atmosphere Atmosphere is rich in hydrogen and methane Methane gas and ice are responsible for the blue color of Uranus’s atmosphere Figure 9.17, Figure 9.18 The Outer Planets

Uranus Uranus’s Interior Uranus’ Rotation Uranus’s interior probably contains water, methane, and ammonia Uranus’ Rotation Uranus spins on its side It is believed that long ago a very large object smashed into this planet.  The crash was so powerful that it completely changed the direction of Uranus' spin Figure 9.19 The Outer Planets

Uranus Uranus’s Rings and Moons Rings Moons Encircled by a set of narrow rings composed of meter-sized objects These objects are very dark, implying they are rich in carbon particles or organic-like materials Moons Uranus has 5 large moons and several small ones Moons probably composed of ice and rock and many show heavy cratering Miranda is very unique in that it appears to have been torn apart and reassembled Figure 9.20, Figure 9.21 The Outer Planets

The Outer Planets

Neptune Introduction Neptune’s Structure Neptune is the outermost of the Jovian giants and similar in size to Uranus A deep blue world with cloud bands and vortex structures Neptune was discovered from predictions made by John C. Adams and Urbain Leverrie, who calculated its orbit based on disturbances in Uranus’s orbit Neptune’s Structure Neptune’s interior is probably similar to Uranus’s – mostly ordinary water surrounded by a thin atmosphere rich in hydrogen and its compounds and probably has a rock/iron core Figure 9.23 The Outer Planets

Neptune Neptune’s Atmosphere Neptune’s blue, like Uranus, comes from methane in its atmosphere Neptune has cloud belts Neptune’s winds are extremely fast reaching speeds of 2200 km/hr and creating visible vortex structures Figure 9.24 The Outer Planets

The Outer Planets

Neptune Neptune’s Rings and Moons Rings Neptune, like the other giant planets, has rings They are probably the debris from small satellites or comets that have collided and broken up The rings are not distributed uniformly around the ring indicating they are relatively new Figure 9.25 The Outer Planets

Neptune Neptune’s Rings and Moons (continued) Moons Neptune has six small moons orbiting close to the planet and two moons farther out One of the two is Triton Triton is large enough and far enough from the others to retain an atmosphere Triton has some craters with dark steaks extending from them – at least one of which originates from a geyser caught in eruption by the passing Voyager II The material in the geyser is thought to be a mixture of nitrogen, ice and carbon compounds heated beneath the surface by sunlight until it expands and bursts to the surface Figure 9.26 The Outer Planets

The Outer Planets

Pluto Survey Discovered by Clyde Tombaugh in 1930 by scanning millions of star images over the course of a year Pluto’s large distance and very small size makes it difficult to study, even in the largest telescopes In 1978, James Christy discovered Charon, Pluto’s moon The orbiting combination of Pluto and Charon allows an accurate measurement of their masses – Pluto is the least massive planet Figure 9.27 The Outer Planets

Pluto Survey (continued) Pluto is 1/5 the diameter of Earth Charon is relatively large, being about ½ Pluto’s diameter From these masses and diameters, Pluto is an object of water, ice, and rock Very little is known of Pluto’s surface Pluto was once thought to be a moon of Neptune that escaped; now it is thought Neptune captured Pluto, a remnant planetesimal Figure 9.28 The Outer Planets

The Outer Planets