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Chapter 11: Jupiter Giant of the Solar System

Chapter 11: Jupiter Giant of the Solar System. Differences from terrestrial planets Atmosphere Structure and Composition Magnetosphere Satellites. After completing this chapter, you should be able to:. compare the general physical properties of Jupiter/Earth.

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Chapter 11: Jupiter Giant of the Solar System

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  1. Chapter 11: JupiterGiant of the Solar System • Differences from terrestrial planets • Atmosphere • Structure and Composition • Magnetosphere • Satellites

  2. After completing this chapter, you should be able to: • compare the general physical properties of Jupiter/Earth. • compare orbital and rotational properties of Jupiter/Earth. • describe atmosphere, hydrosphere, lithosphere, magnetosphere, and biosphere of Jupiter and compare to Earth. • describe Jupiter's cycle of visibility as seen from Earth. • explain why Jupiter's atmosphere is so different from Earth's. • describe Jupiter's ring system. • describe physical properties/origin of Galilean satellites. • explain the origin of Io's volcanoes, Europa’s surface.

  3. Jupiter, Saturn, Uranus, Neptune:The Jovian Planets • Outer or giant or jovian planets. • Over 1400 Earths could fit inside Jupiter • Composed primarily of lighter ices, liquids, gases. • Do not have solid surfaces; more like vast, ball-shaped oceans with much smaller, dense cores at their centers. • Extensive satellite and ring systems.

  4. Planet Properties:Relative Mass of Planets

  5. Planet PropertiesAverage Distance from Sun

  6. Planet Properties:Planetary Densities

  7. Chemistry of Giant Planets • Jupiter & Saturn nearly same chemical makeup as Sun. • primarily hydrogen and helium • by mass: 75% hydrogen, 25% helium • Gas compressed in interior until hydrogen liquifies. • Uranus and Neptune are smaller, attracted less hydrogen and helium. • All have interior core composed of rock, metal, and ice; approximately 10 x mass of Earth. • Chemistry dominated by hydrogen, oxygen in form of H2O (water and water ice) • Reducing chemistry • Atmospheres hydrogen-based gases: CH4 (methane) or NH3 (ammonia) or more complex

  8. Jupiter Fact Sheet • Diameter: 142,800 km (88,736 miles, 11.2 x Earth, 1/10 x Sun) • Mass: 318 x Earth (~1/1000 x Sun) • Density: 1.33 g/cm3 (H2O=1, Earth = 5.5) • Length of Day: 9 hrs 55 min • Length of year: 12 Earth years • Average Distance from Sun: 5.2 AU (483 million miles) • Tilt of Axis: 3.1o • Escape Velocity: 60 km/s • Distance across the Great Red Spot: 40,000 km (~2xEarth’s diameter) • Temperature at Cloud Tops: 124 K • Temperature at core: 20,000 K • Rings: 1, very thin • Satellites: 28 known

  9. Two Object Solar System? • The Sun and Jupiter. • Jupiter has more mass than all of the other objects in solar system combined. • Its gravity: • moves comets into new orbits, • helps keep asteroids in place, • may have created the Oort Cloud of comets, • controls a system of 28 moons • Its tidal pull has: • kept Io molten for billions of years • probably provided Europa with a deep, liquid ocean • Its atmosphere has: • storm swirls larger than the entire Earth • winds that move at over 400 km/hr faster than interior

  10. View from Earth • Closest of Jovian planets to Earth (~ 4AU at its nearest). • Fourth brightest object • brightest when near opposition • up to 50” across • Earth-based telescopes • distinct, multi-colored bands across surface; large reddish area in southern hemisphere • satellites • intense bursts of radio energy

  11. Viewing Jupiter • Oppositions occur every 399 days, so Jupiter is nearest the Earth and brightest once each year. • Because of its great distance from the Earth, its brightness does not vary greatly. • It moves eastward through approximately one constellation of the zodiac each year, because it takes just under 12 years to orbit the Sun. • Jupiter's four large moons (Galilean satellites) are easily visible through a small telescope and even binoculars. • The changing positions of these moons can be seen during one night's observations.

  12. Rotation Rate • No solid surface features to observe. • Cloud features in upper atmosphere move at different rates, depending on latitude, activity. • Near equator: 9 hr 50 m period • Closer to poles: 9 hr 55 m period (globe) • Magnetosphere-related radiation • 9 hr 55 m period • Observed flattening too small for planet composed entirely of hydrogen and helium.

  13. Questions • How do observations of magnetosphere allow astronomers to measure the rotation rate of a planet’s interior? • What is differential rotation? How is it observed on Jupiter? • What does Jupiter’s degree of flattening tell us about its interior?

  14. View from Space • Pioneer 10 and Pioneer 11 (launched 1972, 1973) were first spacecraft to visit outer planets. • navigate asteroid belt • study charged particles and magnetic field • photograph “surface” • Voyager 1 and Voyager 2 launched in 1977. • Designed to study Jupiter and Saturn; both still transmitting data as they travel toward boundary of solar system and into interstellar space. • Voyager 2 passed • within 80,000 km of Uranus (within 16 km of planned target) and • 5000 km above Neptune’s clouds. • Galileo launched in 1989; arrived December, 1995.

  15. Voyager Missions Path through the Solar System

  16. Jupiter Highlights of Voyager Mission • Found 3 new satellites. • Io - active volcanism. • Discovered zones of aurora. • Discovered rings.

  17. Galileo ProjectThe Moon, Asteroids, Jupiter, Io, and Europa • Launched in 1989 from space shuttle Atlantis. • Orbiter and atmospheric probe

  18. Galileo Highlights • Discovery of an intense new radiation belt approximately 50,000 km (31,000 miles) above Jupiter's cloud tops. • Jovian wind speeds in excess of 600 km/hr (> 400 mph) detected. • Far less water was detected in Jupiter's atmosphere than estimated from earlier Voyager observations and from models of the Comet Shoemaker-Levy 9 impact. • Far less lightning activity than anticipated (about 10% of that found in an equal area on Earth). Individual lightning events, however, are about ten times stronger on Jupiter than the Earth. • Helium abundance in Jupiter is very nearly the same as its abundance in the Sun (24% compared to 25%). • Extensive resurfacing of Io's surface due to continuing volcanic activity since the Voyagers flew by in 1979. • Preliminary data support the tentative identification of intrinsic magnetic fields for both Io and Ganymede. • Evidence for liquid water ocean under Europa's surface.

  19. Cassini’s View of Jupiter • Jupiter in three wavelengths • left: blue (visible) • middle: ultraviolet • right: infrared

  20. Interior Structure • A rough model of Jupiter's internal structure can be deduced from the planet's mass, density, rotation, and shape. • Jupiter appears to be highly differentiated with a relatively small rocky and/or metallic core, perhaps the size of Earth and with ~10 x Earth’s mass.

  21. Jupiter’s Internal Structure

  22. Jupiter’s Interior

  23. Jupiter: Composition • Interior composition: mostly simple molecules of hydrogen, liquid form. • Under the cloud layers, as the pressure increases, the hydrogen changes to liquid hydrogen. • Further increases in pressure change liquid hydrogen to liquid metallic hydrogen. • Core composition: heavier, rocky and metal elements.

  24. Jupiter’s Heat Engine infrared wavelengths visible wavelengths Atmospheric motions appear to be driven by internal and external heating.

  25. Jupiter: Heat Sources • Atmospheric motions driven by internal and external heating. • External • Solar energy • Internal • Primordial heat generated during formation by collapse of materials onto core. • Contraction slow shrinking of planet after formation • Jupiter radiates about 1.6 times as much energy into space as it receives from the Sun.

  26. Jupiter’s Internal Motions • The drawing illustrates a kind of global motion typical of motions in both the atmosphere and the interior of a planet. • Material rises from warmest region, and moves in a roiling motion (like boiling of a pot). • Shown are three different cells of activity in the atmosphere where the air turns over (depicted by red sheets). • In the interior of Jupiter, the liquid layers are warm enough to move in this fashion.

  27. More on Interior Motions The drawing shows layered cylinders of material, in motion, rolling in different directions. This pattern may be in operation with the tips of cylinders corresponding to the striped pattern of clouds seen in the atmosphere.

  28. Questions: Internal Structure • What is thought to lie beneath Jupiter’s clouds? • Why do we think this? • Explain a theory that accounts for the unexpectedly high temperatures observed at Jupiter’s cloud tops.

  29. Atmosphere

  30. Atmosphere: Composition • Jupiter has an extremely dense atmosphere. • Its composition is more like the Sun than any of the terrestrial planets. • Hydrogen - 86%. • Helium - 13%. • Methane (CH4) - trace. • Ammonia (NH3) - trace. • Water (H2O) - trace. • Believed that the bulk of the interior has similar composition. • This property makes it quite different than the terrestrial planets and explains its relatively low bulk density.

  31. Jupiter’s Cloud Patterns • Pattern of clouds in white, brown, and orange. • Other shapes include eddy shapes, white ovals, brown ovals, and brown barges. • Eddies and white ovals are outlined in this picture. • Form in stripes and move across face of Jupiter. • Stripes similar to those found on all the giant planets.

  32. Cloud Layers of Jupiter • Three different layers of clouds or clouddecks. • Composition of clouddecks. • 1st: ammonia. • 2nd: ammonium hydrosulfide (ammonia & sulfur) • 3rd: ordinary water clouds

  33. Atmosphere: Circulation • Rapid rotation rate causes planet's atmosphere to • bulge at the equator and • be flattened at the poles. • Rotation rate is greater at the equator than at the poles (differential rotation). • Jupiter's rapid rotation deflects rising and sinking currents of gases (Coriolis effect) into strong zonal flows of winds moving east and west. • somewhat like super jet streams on Earth. • The dark belts are bands of sinking, cooler gases, and the light zones are bands of rising, warmer gases. • Equivalent to Earth’s high and low pressure systems.

  34. Global Circulation Circulation of the Jovian atmosphere. The global circulation pattern shown here indicates the location and designations of the belts and zones in Jupiter's cloud layer. (NASA)

  35. Belts and Zones Motions in the Jovian atmosphere. These drawings indicate both the horizontal (left) and vertical (right) circulation in the clouds of Jupiter. (NASA)

  36. Belts and Zones Wind flow patterns in Jupiter’s belts and zones

  37. Atmosphere: Colors • Colors are caused by trace amounts of organic, sulfur, and/or hydrogen molecules which absorb sunlight at different wavelengths. • A great deal of turbulence occurs at the interface between belts and zones. • These are regions of large jovian storms.

  38. Storms: The Great Red Spot The Great Red Spot is thought to be a hurricane which has been raging on Jupiter for well over 300 years. High-pressure region with high, cold cloud tops (CCW rotation).

  39. Great Red Spot

  40. Great Red Spot HST images of Great Red Spot over a seven year period.

  41. Storms: White Ovals Collections of white clouds, grouped together into an oval shape; commonly found in all regions of Jupiter’s atmosphere.

  42. White Spots vs. GRS • High pressure storms. • Compared to Great Red Spot (GRS) • Lower in the atmosphere than GRS. • Smaller than GRS. • Do not last as long as GRS.

  43. Low pressure storms. Lowest in the atmosphere. actually holes in atmosphere Appear around 20oN latitude. Short-lived compared to GRS Storms: Brown Barges

  44. Atmosphere: Origin and Evolution • Jupiter's atmosphere is thought to be a remnant of Solar System formation. • Evolved very little since initial formation. • That is why planetary scientists feel it is extremely important to study it. • It may be somewhat similar to Earth's primary atmosphere.

  45. Questions: Atmosphere • Why has Jupiter retained most of its original atmosphere? • List some similarities and differences between Jupiter’s belts, zones, and spots and weather systems on Earth. • What is the Great Red Spot? • What is the cause of the colors in Jupiter’s atmosphere?

  46. Magnetosphere • Jupiter has an extensive magnetosphere about 10 time stronger than the Earth's. • This strong magnetic field is probably caused by Jupiter's very rapid rotation and its considerable liquid metallic hydrogen core. • Its magnetic field extends far out into space in a sheet structure centered on the plant's equator. • Jupiter has extremely powerful (and deadly) radiation belts circling the planet. They are much more forceful than Earth's.

  47. Jupiter’s Magnetosphere • Jupiter's magnetosphere is biggest thing in entire solar system. • Big enough to hold all of Jupiter's moons or Sun itself. • Tail extends to Saturn. • From Earth, would appear as large as the full moon. • High levels of energetic particles trapped in regions of magnetosphere, similar to Earth’s Van Allen radiation belts. • New region found by Galileo in uppermost atmosphere 10 x Van Allen in strength. • Donut-shaped cloud inside the magnetosphere coincides with Io. • Jupiter lights up with very beautiful aurora. Jupiter also makes radio signals and other waves (whistler waves, chorus and hiss).

  48. Jupiter’s Magnetosphere

  49. Model of Jupiter’s Magnetosphere Model of magnetosphere showing interaction with solar wind and Io torus.

  50. The Io Torus The Io plasma torus is the result of material being ejected from Io's volcanoes and swept up by Jupiter's rapidly rotating magnetic field. Spectroscopic analysis indicates that the torus is composed primarily of sodium and sulfur atoms.

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