1. Chapter 7 Earth and the Terrestrial Worlds
Insert ECP6 Chapter 7 Opener

2. Mercury Craters Smooth plains Cliffs

3. Venus Volcanoes Few craters
Radar view of a twin-peaked volcano

4. Mars Some craters Volcanoes Riverbeds?
Insert ECP6 Figure 7.26

5. Moon Craters Smooth plains

6. Earth Volcanoes Craters Mountains Riverbeds

7. Why have the planets turned out so differently, even though they formed at the same time from the same materials?

8. 9.1 Earth as a Planet Our goals for learning:
Why is Earth geologically active?
What processes shape Earth’s surface?
How does Earth’s atmosphere affect the planet?

9. Why is Earth geologically active?

10. Earth’s Interior Core: Highest density; nickel and iron
Mantle: Moderate density; silicon, oxygen, etc.
Crust: Lowest density; granite, basalt, etc.

11. Terrestrial Planet Interiors
Applying what we have learned about Earth’s interior to other planets tells us what their interiors are probably like.

12. Why do water and oil separate?
Water molecules repel oil molecules electrically.
Water is denser than oil, so oil floats on water.
Oil is more slippery than water, so it slides to the surface of the water.
Oil molecules are bigger than the spaces between water molecules.

13. Why do water and oil separate?
Water molecules repel oil molecules electrically.
Water is denser than oil, so oil floats on water.
Oil is more slippery than water, so it slides to the surface of the water.
Oil molecules are bigger than the spaces between water molecules.

14. Differentiation Gravity pulls high-density material to center.
Lower-density material rises to surface.
Material ends up separated by density.

15. Thought Question
What is necessary for differentiation to occur in a planet?
It must have metal and rock in it.
It must be a mix of materials of different density.
Material inside must be able to flow.
All of the above
B and C

16. Thought Question
What is necessary for differentiation to occur in a planet?
It must have metal and rock in it.
It must be a mix of materials of different density.
Material inside must be able to flow.
All of the above
B and C

17. Lithosphere
A planet’s outer layer of cool, rigid rock is called the lithosphere.
It “floats” on the warmer, softer rock that lies beneath.

18. Thought Question Do rocks s-t-r-e-t-c-h?
No. Rock is rigid and cannot deform without breaking.
Yes, but only if it is molten rock.
Yes. Rock under strain may slowly deform.

19. Thought Question Do rocks s-t-r-e-t-c-h?
No. Rock is rigid and cannot deform without breaking.
Yes, but only if it is molten rock.
Yes. Rock under strain may slowly deform.

20. Strength of Rock
Rock stretches when pulled slowly but breaks when pulled rapidly.
The gravity of a large world pulls slowly on its rocky content, shaping the world into a sphere.

21. Heat Drives Geological Activity
Convection: Hot rock rises, cool rock falls.
One convection cycle takes 100 million years on Earth.

22. Sources of Internal Heat
Gravitational potential energy of accreting planetesimals
Differentiation
Radioactivity

23. Heating of Interior over Time
Accretion and differentiation when planets were young
Radioactive decay is most important heat source today.

24. Cooling of Interior
Convection transports heat as hot material rises and cool material falls.
Conduction transfers heat from hot material to cool material.
Radiation sends energy into space.

25. Thought Question What cools off faster?
A grande-size cup of Starbucks coffee
A teaspoon of cappuccino in the same cup

26. Thought Question What cools off faster?
A grande-size cup of Starbucks coffee
A teaspoon of cappuccino in the same cup

27. Thought Question What cools off faster? A big terrestrial planet
A tiny terrestrial planet

28. Thought Question What cools off faster? A big terrestrial planet
A tiny terrestrial planet

29. Role of Size Smaller worlds cool off faster and harden earlier.
The Moon and Mercury are now geologically “dead.”

30. Surface Area-to-Volume Ratio
Heat content depends on volume.
Loss of heat through radiation depends on surface area.
Time to cool depends on surface area divided by volume:
Larger objects have a smaller ratio and cool more slowly.

31. Planetary Magnetic Fields
Moving charged particles create magnetic fields.
A planet’s interior can create magnetic fields if its core is electrically conducting, convecting, and rotating.

32. Earth’s Magnetosphere
Earth’s magnetic field protects us from charged particles from the Sun.
The charged particles can create aurorae (“Northern lights”).

33. Thought Question
If the planet core is cold, do you expect it to have magnetic fields?
Yes. Refrigerator magnets are cold, and they have magnetic fields.
No. Planetary magnetic fields are generated by moving charges around, and if the core is cold, nothing is moving.

34. Thought Question
If the planet core is cold, do you expect it to have magnetic fields?
Yes. Refrigerator magnets are cold, and they have magnetic fields.
No. Planetary magnetic fields are generated by moving charges around, and if the core is cold, nothing is moving.

35. Special Topic: How do we know what’s inside a planet?
P waves push matter back and forth.
S waves shake matter side to side.

36. Special Topic: How do we know what’s inside a planet?
P waves go through Earth’s core, but S waves do not.
We conclude that Earth’s core must have a liquid outer layer.

37. What processes shape Earth’s surface?

38. Geological Processes Impact cratering Volcanism Tectonics Erosion
Impacts by asteroids or comets
Volcanism
Eruption of molten rock onto surface
Tectonics
Disruption of a planet’s surface by internal stresses
Erosion
Surface changes made by wind, water, or ice

39. Impact Cratering
Most cratering happened soon after the solar system formed.
Craters are about 10 times wider than the objects that made them.
Small craters greatly outnumber large ones.

40. Impact Craters
Meteor Crater (Arizona)
Tycho (Moon)

41. Volcanism
Volcanism happens when molten rock (magma) finds a path through lithosphere to the surface.
Molten rock is called lava after it reaches the surface.

42. Outgassing
Volcanism also releases gases from Earth’s interior into the atmosphere.

43. Tectonics
Convection of the mantle creates stresses in the crust called tectonic forces.
Compression forces make mountain ranges.
A valley can form where the crust is pulled apart.

44. Plate Tectonics on Earth
Earth’s continents slide around on separate plates of crust.
Plate Tectonics on Earth

45. Erosion
Erosion is a blanket term for weather-driven processes that break down or transport rock.
Processes that cause erosion include
Glaciers
Rivers
Wind

46. Erosion by Water
The Colorado River continues to carve the Grand Canyon.

47. Erosion by Ice
Glaciers carved the Yosemite Valley.

48. Erosion by Wind
Wind wears away rock and builds up sand dunes.

49. Erosional Debris
Erosion can create new features by depositing debris.

50. How does Earth’s atmosphere affect the planet?

51. Effects of Atmosphere on Earth
Erosion
Radiation protection
Greenhouse effect
Makes the sky blue!

52. Radiation Protection
All X-ray light is absorbed very high in the atmosphere.
Ultraviolet light is absorbed by ozone (O3).

53. The Greenhouse Effect

54. Earth’s atmosphere absorbs light at most wavelengths.

55. Greenhouse effect:
Certain molecules let sunlight through but trap escaping infrared photons.
(H2O, CO2, CH4)
The Greenhouse Effect

56. A Greenhouse Gas Any gas that absorbs infrared
Greenhouse gas: molecules with two different types of elements (CO2, H2O, CH4)
Not a greenhouse gas: molecules with one or two atoms of the same element (O2, N2)

57. Greenhouse Effect: Bad?
Because of the greenhouse effect, Earth is much warmer than it would be without an atmosphere…but so is Venus.

58. Thought Question Why is the sky blue?
The sky reflects light from the oceans.
Oxygen atoms are blue.
Nitrogen atoms are blue.
Air molecules scatter blue light more than red light.
Air molecules absorb red light.

59. Thought Question Why is the sky blue?
The sky reflects light from the oceans.
Oxygen atoms are blue.
Nitrogen atoms are blue.
Air molecules scatter blue light more than red light.
Air molecules absorb red light.

60. Why the sky is blue
Atmosphere scatters blue light from the Sun, making it appear to come from different directions.
Sunsets are red because less of the red light from the Sun is scattered.

61. What have we learned? Why is Earth geologically active?
Earth retains plenty of internal heat because it is large for a terrestrial planet.
That heat drives geological activity, keeping the core molten and driving geological activity.
The circulation of molten metal in the core generates Earth’s magnetic field.

62. What have we learned? What geological processes shape Earth’s surface?
Impact cratering, volcanism, tectonics, and erosion
How does Earth’s atmosphere affect the planet?
Erosion
Protection from radiation
Greenhouse effect

63. 7.2 Mercury and the Moon: Geologically Dead
Our goals for learning:
Was there ever geological activity on the Moon or Mercury?

64. Was there ever geological activity on the Moon or Mercury?

65. Moon
Some volcanic activity 3 billion years ago must have flooded lunar craters, creating lunar maria.
The Moon is now geologically dead.

66. Cratering of Mercury
Mercury has a mixture of heavily cratered and smooth regions like the Moon.
The smooth regions are likely ancient lava flows.

67. Cratering of Mercury
The Caloris Basin is the largest impact crater on Mercury.
Region opposite the Caloris Basin is jumbled from seismic energy of impact.

68. Tectonics on Mercury
Long cliffs indicate that Mercury shrank early in its history.

69. What have we learned?
Was there ever geological activity on the Moon or Mercury?
Early cratering on the Moon and Mercury is still present, indicating that activity ceased long ago.
Lunar maria resulted from early volcanism.
Tectonic features on Mercury indicate early shrinkage.

70. 7.3 Mars: A Victim of Planetary Freeze-Drying
Our goals for learning:
What geological features tell us that water once flowed on Mars?
Why did Mars change?

71. Mars versus Earth 50% Earth’s radius, 10% Earth’s mass
1.5 AU from the Sun
Axis tilt about the same as Earth
Similar rotation period
Thin CO2 atmosphere: little greenhouse
Main difference: Mars is SMALLER

72. Seasons on Mars
Seasons on Mars are more extreme in the southern hemisphere because of its elliptical orbit.

73. Storms on Mars
Seasonal winds on Mars can drive huge dust storms.

74. What geological features tell us that water once flowed on Mars?

75. The surface of Mars appears to have ancient riverbeds.

76. The condition of craters indicates surface history.
Eroded crater
The condition of craters indicates surface history.

78. Volcanoes…as recent as 180 million years ago…

79. Past tectonic activity…

80. Inset shows hypothetical ancient ‘water line’ for Gusev Crater where Spirit landed
Opportunity

81. 2004 Opportunity rover provided strong evidence for abundant liquid water on Mars in the distant past.
How could Mars have been warmer and wetter in the past?

82. Today, most water lies frozen underground (blue regions).
Some scientists believe accumulated snowpack melts carve gullies even today.

83. Why did Mars change?

84. Climate Change on Mars
Mars has not had widespread surface water for 3 billion years.
The greenhouse effect probably kept the surface warmer before that.
Somehow Mars lost most of its atmosphere.

85. Climate Change on Mars
Magnetic field may have preserved early Martian atmosphere.
Solar wind may have stripped atmosphere after field decreased because of interior cooling.

86. What have we learned?
What geological features tell us that water once flowed on Mars?
Dry riverbeds, eroded craters, and rock-strewn floodplains all show that water once flowed on Mars.
Mars today has ice, underground water ice, and perhaps pockets of underground liquid water.
Why did Mars change?
Mars’s atmosphere must have once been much thicker for its greenhouse effect to allow liquid water on the surface.
Somehow Mars lost most of its atmosphere, perhaps because of a declining magnetic field.

87. 7.4 Venus: A Hothouse World
Our goals for learning:
Is Venus geologically active?
Why is Venus so hot?

88. Is Venus geologically active?

89. Cratering on Venus
Impact craters, but fewer than Moon, Mercury, Mars

90. Volcanoes on Venus
Many volcanoes

91. Tectonics on Venus
Fractured and contorted surface indicates tectonic stresses

92. Erosion on Venus
Photos of rocks taken by lander show little erosion

93. Does Venus have plate tectonics?
Most of Earth’s major geological features can be attributed to plate tectonics, which gradually remakes Earth’s surface.
Venus does not appear to have plate tectonics, but its entire surface seems to have been “repaved” 750 million years ago.

94. Why is Venus so hot?

95. Why is Venus so hot?
The greenhouse effect on Venus keeps its surface temperature at 470°C.
But why is the greenhouse effect on Venus so much stronger than on Earth?

96. Atmosphere of Venus
Venus has a very thick carbon dioxide atmosphere with a surface pressure 90 times that of Earth.

97. Greenhouse Effect on Venus
Thick carbon dioxide atmosphere produces an extremely strong greenhouse effect.
Earth escapes this fate because most of its carbon and water are in rocks and oceans.

98. Atmosphere of Venus
Reflective clouds contain droplets of sulfuric acid.
The upper atmosphere has fast winds that remain unexplained.

99. Runaway Greenhouse Effect
More evaporation, stronger greenhouse effect
The runaway greenhouse effect would account for why Venus has so little water.
Greater heat, more evaporation

100. Thought Question What is the main reason Venus is hotter than Earth?
Venus is closer to the Sun than Earth.
Venus is more reflective than Earth.
Venus is less reflective than Earth.
The greenhouse effect is much stronger on Venus than on Earth.
Human activity has led to declining temperatures on Earth.

101. Thought Question What is the main reason Venus is hotter than Earth?
Venus is closer to the Sun than Earth.
Venus is more reflective than Earth.
Venus is less reflective than Earth.
The greenhouse effect is much stronger on Venus than on Earth.
Human activity has led to declining temperatures on Earth.

102. What have we learned? Is Venus geologically active?
Its surface shows evidence of major volcanism and tectonics during the last billion years.
There is no evidence for erosion or plate tectonics.
Why is Venus so hot?
The runaway greenhouse effect made Venus too hot for liquid oceans.
All carbon dioxide remains in the atmosphere, leading to a huge greenhouse effect.

103. 7.5 Earth as a Living Planet
Our goals for learning:
What unique features of Earth are important for human life?
How is human activity changing our planet?
What makes a planet habitable?

104. What unique features of Earth are important for life?
Surface liquid water
Atmospheric oxygen
Plate tectonics
Climate stability

105. What unique features of Earth are important for life?
Earth’s distance from the Sun and moderate greenhouse effect make liquid water possible.
Surface liquid water
Atmospheric oxygen
Plate tectonics
Climate stability

106. What unique features of Earth are important for life?
Surface liquid water
Atmospheric oxygen
Plate tectonics
Climate stability
PHOTOSYNTHESIS (plant life) is required to make high concentrations of O2, which produces the protective layer of O3.

107. What unique features of Earth are important for life?
Surface liquid water
Atmospheric oxygen
Plate tectonics
Climate stability
Plate tectonics is an important step in the carbon dioxide cycle.

108. Continental Motion
Motion of continents can be measured with GPS.

109. Continental Motion
Idea of continental drift was inspired by puzzle-like fit of continents.
Mantle material erupts where seafloor spreads.

110. Seafloor Recycling
Seafloor is recycled through a process known as subduction.

111. Plate Motions
Measurements of plate motions tell us past and future layout of continents.

112. Carbon Dioxide Cycle Atmospheric CO2 dissolves in rainwater.
Rain erodes minerals that flow into the ocean.
Minerals combine with carbon to make rocks on ocean floor.

113. Carbon Dioxide Cycle
Subduction carries carbonate rocks down into the mantle.
Rock melts in mantle and outgases CO2 back into atmosphere through volcanoes.

114. Long-Term Climate Change
Changes in Earth’s axis tilt might lead to ice ages.
Widespread ice tends to lower global temperatures by increasing Earth’s reflectivity.
CO2 from outgassing will build up if oceans are frozen, ultimately raising global temperatures again.

115. What unique features of Earth are important for life?
Surface liquid water
Atmospheric oxygen
Plate tectonics
Climate stability
The CO2 cycle acts like a thermostat for Earth’s temperature.

116. These unique features are intertwined:
Plate tectonics creates climate stability.
Climate stability allows liquid water.
Liquid water is necessary for life.
Life is necessary for atmospheric oxygen.
For example: atmospheric oxygen allows life on land; stable climate good for life; water may enable plate tectonics.
How many other connections between these can you think of?

117. How is human activity changing our planet?

118. Dangers of Human Activity
Human-made CFCs in the atmosphere destroy ozone, reducing protection from UV radiation.
Human activity is driving many other species to extinction.
Human use of fossil fuels produces greenhouse gases that can cause global warming.

119. Global Warming
Earth’s average temperature has increased by 0.5°C in the past 50 years.
The concentration of CO2 is rising rapidly.
An unchecked rise in greenhouse gases will eventually lead to global warming.

120. CO2 Concentration
Global temperatures have tracked CO2 concentration for the last 500,000 years.
Antarctic air bubbles indicate the current CO2 concentration is at its highest level in at least 500,000 years.

121. CO2 Concentration
Most of the CO2 increase has happened in the last 50 years!

122. Modeling of Climate Change
Models of global warming that include human production of greenhouse gases are a better match to the global temperature rise.

123. What makes a planet habitable?
Located at an optimal distance from the Sun for liquid water to exist

124. What makes a planet habitable?
Large enough for geological activity to release and retain water and atmosphere

125. Planetary Destiny
Earth is habitable because it is large enough to remain geologically active, and it is at the right distance from the Sun so oceans could form.

126. What have we learned?
What unique features of Earth are important for life?
Surface liquid water
Atmospheric oxygen
Plate tectonics
Climate stability

127. What have we learned? How is human activity changing our planet?
Human activity is releasing carbon dioxide into Earth’s atmosphere, increasing the greenhouse effect and producing global warming.
What makes a planet habitable?
Earth’s distance from the Sun allows for liquid water on Earth’s surface.
Earth’s size allows it to retain an atmosphere and enough internal heat to drive geological activity.