Outline for 21 November Tuesday

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Outline for 21 November (Tuesday)

• Planets and Moons
• Orbits
• Surface and Interior
• Atmosphere
• Rings

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Outline for 21 November (Tuesday)

• Planets and Moons
• Orbits
• Surface and Interior
• Atmosphere
• Rings

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Outline for 21 November (Tuesday)

• Planets and Moons
• Orbits
• Distance from Sun
• Eccentricity
• Distance from controlling object
• Rotation period
• Tidal forces
• Synchronous rotation

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Synchronous Rotation

• Why does it happen?

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Chapter 11

• 4b. Mercury can be seen most easily from Earth
• A) near the Sun, just after sunset or just before
  sunrise.
• B) during a lunar eclipse, when the sky is
  sufficiently dark near the Moon, because Mercury
  is always close to the Moon in our sky.
• C) in the winter, when the ecliptic plane is high
  in the sky at night.
• D) at midnight, when it is high in the sky.

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Chapter 11

• 12b. How often does a solar transit of
  MercuryMercury passing directly across the face
  of the Sun as seen from Earthoccur?
• A) regularly, once every synodic period of
  Mercury, or every 116 days
• B) never
• C) regularly, every sidereal period of Mercury,
  or every 88 days
• D) relatively infrequentlybetween 10 and 20
  times per century

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Chapter 13

• 2q. The length of each of the Martian seasons,
  compared to those on Earth, is
• (a) about the same as Earth because the tilt of
  Mars's spin axis and rotation rate are similar to
  those of Earth.
• (b) about twice as long because of Mars's orbital
  period.
• (c) about half as long as Earth, due to the
  relationship between the Martian period of
  revolution and its synodic period.

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Chapter 13

• 17b. Mars experiences similar seasonal changes to
  those on Earth because
• A) it has about the same shape of elliptical
  orbit as that of the Earth, producing similar
  changes in solar radiation intensity as the
  planet orbits the Sun.
• B) its spin axis is tilted at about the same
  angle to its orbital plane as is the Earth's
  axis.
• C) the length of its day is very close to an
  Earth day.
• D) the length of its year is very close to that
  of Earth.

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Key Terms

• greatest eastern elongation
• greatest western elongation
• solar transit
• prograde rotation
• retrograde rotation
• occultation
• 1-to-1 spin-orbit coupling
• 3-to-2 spin-orbit coupling

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Draw ball and arrow at A, B, C, D
C
D
B
A
Mercurys orbital period is 88 days Mercurys
rotation period is 58 days
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Draw ball and arrow at A, B, C, D
C
D
B
A
Mercurys orbital period is 88 days Mercurys
rotation period is 58 days
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Draw ball and arrow at A, B, C, D
C
D
B
A
88/4 22 days to get to A
Mercurys orbital period is 88 days Mercurys
rotation period is 58 days
22/58 0.375
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Draw ball and arrow at A, B, C, D
First rotate around Mercurys axis. Then move
into position in orbit.
C
0.375 of a full turn
D
B
A
88/4 22 days to get to A
Mercurys orbital period is 88 days Mercurys
rotation period is 58.6 days
22/58 0.375
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Draw ball and arrow at A, B, C, D
C
D
D
B
A
88/4 22 days to get to A
Mercurys orbital period is 88 days Mercurys
rotation period is 58 days
22/58 0.375
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C
1.125 turns
D
0.75 of a full turn
B
1.5 turns
0.375 of a turn
A
A
88/4 22 days to get to A
Mercurys orbital period is 88 days Mercurys
rotation period is 58 days
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Outline for 21 November (Tuesday)

• Planets and Moons
• Orbits
• Surface and Interior
• Atmosphere
• Rings

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Outline for 21 November (Tuesday)

• Planets and Moons
• Surface and Interior
• Core
• What surrounds core
• Rotation period
• Quakes
• Tides
• Craters
• Recycling

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Moon
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The surface of Venus shows no evidence of plate
tectonics

• The surface of Venus is surprisingly flat, mostly
  covered with gently rolling hills
• There are a few major highlands and several large
  volcanoes
• The surface of Venus shows no evidence of the
  motion of large crustal plates, which plays a
  major role in shaping the Earths surface

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Chapter 12

• 80b. On both Earth and Venus some sulfur dioxide
  is removed from the atmosphere to be locked up in
  various rocks and minerals. On Earth this SO2 is
  recycled deep beneath the surface to be outgassed
  by volcanoes and again become part of the
  atmosphere. On Venus this SO2 is not recycled.
  Why this difference?
• A) There are no active volcanoes on Venus.
• B) Venus does not experience the movement of
  tectonic plates.
• C) On Venus, the sulfur dioxide minerals are
  dissolved by acids in the atmosphere.
• D) Because of the higher temperature on Venus,
  the SO2 minerals formed there are different from
  those on Earth, and they are essentially
  permanent and nonrecyclable.

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Chapter 12

• 90b. Tectonic activity on Venus differs from that
  on Earth in that
• A) active crustal deformation appears to be
  completely absent.
• B) the lithosphere appears to be softer or more
  plastic and cannot support the creation and
  motion of solid plates.
• C) the lithosphere appears to be cooler and
  thicker and is therefore too rigid to break up
  into moving plates.
• D) mantle convection appears to be more vigorous
  and has broken the lithosphere into a multitude
  of small plates instead of a few large ones.

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Chapter 14

• 15q. What is believed to be the most important
  source for the internal heat that Saturn radiates
  to space?
• (a) Raindrops of liquid helium.
• (b) The original heat of formation of the planet.
• (c) Decay of radioactive elements in Saturn's
  large, rocky core.

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Chapter 10

• 7q. How do we know the lunar maria (or "seas")
  are younger than the lunar highlands?
• (a) The maria have relatively few craters,
  whereas the highlands are very densely cratered
  from long exposure to incoming meteoroids.
• (b) The maria are still dark, whereas the
  highlands have been lightened by a much longer
  exposure to radiation from the Sun.
• (c) The maria are lower in elevation, whereas the
  highlands have had time to be uplifted by
  tectonic processes.

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Outline for 21 November (Tuesday)

• Planets and Moons
• Orbits
• Surface and Interior
• Atmosphere
• Rings

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Outline for 21 November (Tuesday)

• Planets and Moons
• Atmosphere
• Life
• Shield
• Thickness and gravity
• Temperature and escape
• Greenhouse effect

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Atmospheres

• gravity and escape velocity

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Atmospheres

• gravity and escape velocity

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The climate on Venus followed a different
evolutionary path from that on Earth

• Venuss high temperature is caused by the
  greenhouse effect, as the dense carbon dioxide
  atmosphere traps and retains energy from
  sunlight.
• The early atmosphere of Venus contained
  substantial amounts of water vapor
• This caused a runaway greenhouse effect that
  evaporated Venuss oceans and drove carbon
  dioxide out of the rocks and into the atmosphere

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The climate on Venus followed a different
evolutionary path from that on Earth

• Almost all of the water vapor was eventually lost
  by the action of ultraviolet radiation on the
  upper atmosphere.
• The Earth has roughly as much carbon dioxide as
  Venus, but it has been dissolved in the Earths
  oceans and chemically bound into its rocks

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Earths Atmosphere
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Mars Atmosphere
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Chapter 12

• 12q. The temperature in the atmosphere of Venus
  decreases smoothly with increasing altitude all
  the way from the surface (hottest) to the
  outermost parts of the atmosphere (coolest). What
  does this observation tell us about the
  atmosphere of Venus? (Hint Think about why the
  temperature in the Earth's atmosphere differs
  from this.)
• (a) Venus has no distinct layers of clouds or
  aerosols in its atmosphere.
• (b) Venus has essentially no ozone in its
  atmosphere.
• (c) Venus has essentially no convection in its
  atmosphere.

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Chapter 12

• 34b. Why is the surface of Venus hotter than that
  of Mercury, even though Mercury is much closer to
  the Sun?
• A) Chemical reactions within the thick clouds and
  dense atmosphere are continuously supplying heat
  to the surface.
• B) Continuous volcanic activity releases large
  quantities of hot lava onto the surface.
• C) Venus rotates rapidly, thereby ensuring that
  its entire surface is being heated regularly and
  uniformly.
• D) The thick CO2 atmosphere prevents re-emission
  into space of the heat absorbed from sunlight.

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Chapter 12

• 81b. At what point did the greenhouse effect
  cease to raise the temperature of Venus?
• A) when all the greenhouse gases evaporated
• B) when the radiation from Venus balanced the
  radiation absorbed by Venus
• C) when the CO2 was dissolved in the early
  Venusian oceans
• D) when the greenhouse gases combined with other
  chemicals

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Key Terms

• runaway greenhouse effect
• retrograde rotation
• dust devil
• runaway icehouse effect
• thermal radiation

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Outline for 21 November (Tuesday)

• Planets and Moons
• Orbits
• Surface and Interior
• Atmosphere
• Rings

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Outline for 21 November (Tuesday)

• Planets and Moons
• Rings
• Why they form
• Orbits
• Interaction with Moons

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