Chapter 24 Uranus, Neptune, and Pluto

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1 Chapter 24 Uranus, Neptune, and Pluto Guidepost In the three previous chapters, we have used our tools of comparative planetology to study other worlds, and we continue that theme in this chapter. A second theme running through this chapter is the nature of astronomical discovery. Unlike the other planets in our solar system, Uranus, Neptune, and Pluto were discovered, and the story of their discovery helps us understand how science progresses. As we probe the outer fringes of our planetary system in this chapter, we see strong evidence of smaller bodies that fall through the solar system and impact planets and satellites. The next chapter will allow us to study these small bodies in detail and will give us new evidence that our solar system formed from a solar nebula. 1

2 Outline I. Uranus A. The Discovery of Uranus B. The Motion of Uranus C. The Atmosphere of Uranus D. The Interior of Uranus E. The Rings of Uranus F. The Moons of Uranus G. A History of Uranus II. Neptune A. The Discovery of Neptune B. The Atmosphere and Interior of Neptune C. The Rings of Neptune D. The Moons of Neptune E. The History of Neptune Outline (continued) III. Pluto A. The Discovery of Pluto B. Pluto as a Planet C. The Origin of Pluto and Charon 2

3 Uranus Chance discovery by William Herschel in 1781, while scanning the sky for objects with measurable parallax. Herschel saw Uranus as slightly extended object, about 3.7 arc seconds in diameter. audio link The Motion of Uranus Unusual rotation axis, almost on its side. Axial tilt is possibly the result of large impact during planet formation. One hemisphere has sunlight for decades, then darkness for decades. Sun rises and sets only at equinox AU 97.9 o 3

4 The Atmosphere of Uranus Like other gas giants it has no surface, but a gradual transition from gas phase to fluid interior. 83% hydrogen, 15% helium, 2% methane, ammonia & water vapor. Optical view from Earth shows blue due to methane, absorbing longer wavelengths Cloud structures only visible after artificial computer enhancement of optical images taken from Voyager spacecraft. The Structure of Uranus Atmosphere Upper layer of methane clouds makes planet look blue. Clouds of ammonia, ammonia hydrosulfide and water occur in deeper, warmer layers. Lower cloud layers hard to see because of thick atmosphere above it. Subtle belt-zone structure must be dominated by planet s rotation, not by direction of sun light. 4

5 Planetary Atmospheres (SLIDESHOW MODE ONLY) Cloud Structure of Uranus Hubble Space Telescope image of Uranus shows cloud structures not present during Voyager s passage in Could be the result of seasonal changes of the cloud structures? 5

6 The Interior of Uranus Average density is 1.29 g/cm 3, so it has a larger portion of rock and ice than Jupiter and Saturn. Under intense pressure/temperature, methane can form pure carbon diamonds! Ices of water, methane, and ammonia, mixed with hydrogen and silicates Uranus and Neptune often called ice giants because of icy interior The Magnetic Field of Uranus No metallic core so no magnetic field was expected. But actually, magnetic field of around 75% of Earth s magnetic field strength was discovered. Magnetic field possibly from dynamo effect in layer of liquid-water/ ammonia/methane near the surface Magnetic field is offset from center and inclined from axis of rotation. Rotation period of hr measured by fluctuation in radiation belts trapped in magnetosphere. 6

7 The Magnetosphere of Uranus Rapid rotation and large inclination deform magnetosphere into a corkscrew shape. UV images During Voyager 2 flyby the south pole was pointed towards the sun. Interaction of solar wind with magnetosphere showed bright aurora. The Rings of Uranus Rings of Uranus and Neptune are similar to Jupiter s rings. Confined by shepherd moons and consist of dark material. Apparent motion of star behind Uranus and rings Rings of Uranus were discovered through occultations of a background star 7

8 Uranus s Ring Detection (SLIDESHOW MODE ONLY) The Moons of Uranus 5 largest moons visible from Earth. 10 more discovered by Voyager 2; more are still being found. Dark surfaces, probably ice darkened by dust from meteorite impacts. 5 largest moons are all tidally locked to Uranus. 8

9 Interiors of Uranus s Moons Large rock cores surrounded by icy mantles. The Surfaces of Uranus s Moons (1) Oberon Old, inactive, cratered surface, but probably active past. Long fault across the surface. Dirty water may have flooded floors of some craters. Titania Largest moon Heavily cratered surface, but no very large craters. Active phase with internal melting might have flooded craters. 9

10 2/4/11 The Surfaces of Uranus s Moons (2) Umbriel Dark, cratered surface No faults or other signs of surface activity Ariel Brightest surface of 5 largest moons Clear signs of geological activity Crossed by faults over 10 km deep Possibly heated by tidal interactions with Miranda and Umbriel. Uranus s Moon Miranda Most unusual of the 5 moons detected from Earth Ovoids: Oval groove patterns, 20 km high cliff near the equator probably associated with convection currents in the Surface features are old; Miranda is no longer geologically active. mantle, but not with impacts. 10

11 Neptune Discovered in 1846 at position predicted from gravitational disturbances on Uranus s orbit. Blue-green color from methane in the atmosphere (like Uranus.) 4 times Earth s diameter; 4% smaller than Uranus. The Atmosphere of Neptune The Great Dark Spot Cloud-belt structure with high-velocity winds, but origin not well understood. White cloud features of methane ice crystals Darker cyclonic disturbances, similar to Great Red Spot on Jupiter, but not long-lived. Rotation period of 16 hr measured by Great Dark Spot moving counterclockwise. 11

12 The Magnetic Field of Neptune Heavy element core, like Uranus, does not produce a magnetic field. Magnetic field about 50% of Earth s field, probably caused by dynamo effect in fluid mantle. Magnetic field is offset from center and inclined from axis of rotation. The Rings of Neptune Ring material must be regularly resupplied by dust from meteorite impacts on the moons. Interrupted between denser segments (arcs) Made of dark dusty material, visible in forwardscattered light. Focused by small shepherd moons embedded in the ring structure. 12

13 The Moons of Neptune Two moons (Triton and Nereid) visible from Earth; 6 more discovered by Voyager 2 Unusual orbits: Triton: Only satellite in the solar system orbiting clockwise, ( backward ). Nereid: Highly eccentric orbit; very long orbital period (359.4 d). Astronomers think a violent collision or capture may caused these strange orbits. The Surface of Triton Very low temperature at near absolute zero! Triton can hold a thin atmosphere of nitrogen and some methane Surface composed of ices: nitrogen, methane, carbon monoxide, carbon dioxide. Possibly cyclic nitrogen ice deposition and revaporizing on Triton s south pole, similar to CO 2 ice polar cap cycles on Mars. Dark smudges on the nitrogen ice surface, probably due to methane rising from below surface, forming carbon-rich deposits when exposed to sun light. 13

14 The Surface of Triton (2) One of few moons in solar system with geologic activity: surface features probably less than 100 million years old. Large basins might have been flooded many times by liquids from the interior. Icy version of greenhouse effect may be one of the heat sources for Triton s geological activity. Pluto Discovered 1930 by Clyde Tombaugh. Existence predicted from orbital disturbances of Neptune, but Pluto is actually too small to cause those disturbances. 14

15 Pluto as a Planet No surface features visible from Earth. about 65% of size of Earth s Moon. Elliptical orbit (30-50 AU); occasionally closer to the sun than Neptune. Orbit highly inclined (17 o ) to other planets orbits Neptune and Pluto will never collide; they are in 3:2 orbital resonance. Surface covered with nitrogen ice, frozen methane, and carbon monoxide. Daytime temperature (50 K) enough to vaporize some nitrogen and carbon dioxide to form a very thin atmosphere. Pluto s Moon Charon Discovered in 1978; about half the size and 1/12 the mass of Pluto itself. Tidally locked to Pluto in a nearly circular orbit. Hubble Space Telescope image Two other small moons found by Hubble in

16 Pluto and Charon Orbit highly inclined against orbital plane. From orbital distance and orbital period, Pluto s mass is found about one-fifth of Earth s mass. Density is about 2 g/cm 3 for both Pluto and Charon. Surface is about 35% ice and 65% rock. Large orbital inclinations cause big seasonal changes, like Uranus. The Origin of Pluto and Charon Probably very different history than neighboring Jovian planets. Older theory suggests that Pluto and Charon formed as moons of Neptune, ejected by interaction with massive planetesimal. Theory mostly abandoned today since such interactions are unlikely. Modern theory suggests Pluto and Charon are members of Kuiper Belt of small, icy objects. Collision between Pluto and Charon may have caused the peculiar orbital patterns and large inclination of Pluto s rotation axis. New Horizons spacecraft will reach Pluto in July,

17 New Terms occultation ovoid 17

2007 Pearson Education Inc., publishing as Pearson Addison-Wesley. The Jovian Planets

2007 Pearson Education Inc., publishing as Pearson Addison-Wesley. The Jovian Planets The Jovian Planets The Jovian planets are gas giants - much larger than Earth Sizes of Jovian Planets Planets get larger as they get more massive up to a point... Planets more massive than Jupiter are