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73 Cards in this Set
- Front
- Back
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Terrestrial Planets
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Mercury, Venus, Earth, Mars
Low mass, high density |
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Jovian Planets
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Jupiter, Saturn, Uranus, Neptune
high mass, low density |
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Moons
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natural satellites, more than 100 in the solar system
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Asteroids
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small, rocky metallic bodies that orbit the sun
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Comets
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small, rocky, icy bodies that orbit the sun
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Asteroid Belt
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Between Mars and Jupiter
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Motion of Solar System Bodies
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Counterclockwise in nearly the same place
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Age of the sun
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5 billion years
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Age of Solar System
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4.56 billion years
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Solar Nebula Theory
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proton sun and accretion disk
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Condensation and Accretion
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Small particles stick together to form larger particles
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Particles from smallest to largest
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Grain, Planetesimal, Planetary body
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Planet buliding must begin before the sun is fully formed. Why?
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Small particles are pushed outward easily by radiation and solar wind
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Composition of Solar Nebula
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3/4 hydrogen
1/4 helium 2% heavier elements (1% Oxygen, .3% Carbon, .3% Neon) |
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Primary Planet building materials
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3/4 ices
1/4 rocks and metals |
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Condensation Sequence
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rocks and metals condense at 1500K, ices at 200K
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Formation Timeline
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Jupiter and Saturn Form, then sun, then terrestrial planets
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Asteroid Belt Formation
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Jupiters early formation perturbed nearby planetesimals. They collided and fragmented
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Kuiper Belt
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comet belt of icy and rocky planetesimals accreted beyond Neptune
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Oort Cloud
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icy, rocky planetesimals accreted in the Jovian Planet region
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Moons
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Captured planetesimals or form in mini accretion disks around planets
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Extrasolar Planets
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planets orbiting other stars
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How do we detect them?
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Indirectly by means of radial velocity
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What can we see by the radial velocity curve?
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Semi-major axis and minimum mass
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What types of planets do we find the most of?
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high mass close to stars "hot jupiters"
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How did we find the composition of Earth?
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evidence from seismic waves-s waves pass through liquids
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Differentiation
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sorting of materials by density inside a molten body
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What is driving plate tectonics?
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Convection cells in the mantle
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Atmospheric Pressure at sea level
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14.7 lb/in (1 ATM)
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Composition of dry air
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78% nitrogen
21% oxygen 1% argon .03% Carbon dioxide |
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Evolution of Earth's Atmosphere
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Atmosphere was once mostly CO2, and water vapor. Earth cooled and the water vapor condensed. CO2 dissolved in the water to form a carbonate which calcium reacted with to form limestone.
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What causes Earth's magnetic field?
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Convection cells in the outer core and rotation
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What distorts our magnetic fields? What does this cause?
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Solar wind; aurorae
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Requirements for a strong magnetic field
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Liquid conducting interior zone
Rapid rotation |
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the moon's age of bright, rough highlands
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very old
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dark, smooth lowlands
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slightly old
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bright rayed craters
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young
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Structure of moon
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small iron core
rocky mantle thick rocky crust that is thinner on the side that faces Earth |
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Moon Composition
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low in ice, identical oxygen isotope ratios
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Moons affect on the tides
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bulge on the far sides of earth-2 high tides and 2 low tides
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Sun affect on the tides
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1/3 of the tide affect
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Spring tides
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most extreme, moon and sun work together since we're in a line, at the full and new moon
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Neap tides
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less extreme, moon and sun work against one another since they are at a 90 degree angle, at the first and third quarter moon
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Earth carries tidal bulge ahead of the moon. What does this cause?
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Day's increase by .002 seconds every 100 years
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Earth transfers spin to the moon
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Distance increases by 10 feet every 100 years
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Eventually what will be the same when it comes to the Earth and Moon?
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Earths rotational period and moons orbital period
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Mercury surface features
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old surface with lots of impact craters and polar ice caps
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Structure and composition of mercury
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high density center, low density exterior, large metallic core, thin crust and mantle
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Surface features of Venus
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always clouded, gently rolling plains, large shield volcanoes because of no plate tectonics
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Atmosphere
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92 ATM 96% CO2, 4% N2
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Mars Surface Features
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polar ice caps (winter and summer), canyon, shield volcanoes, dry river beds
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Atmosphere
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less than 0.01 ATM 95% CO2, 3% N2, dust storms
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Moons
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Phobos, Deimos-captured asteroids
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Jupiters distinguishing features
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banded appearance, great red spot
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Structure of Jupiter
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small rocky core, liquid ice layer, liquid metallic hydrogen layer
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Composition
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mostly hydrogen and helium
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Moons
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Io, Europa, Ganymede, Callisto
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Trends in moons
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high density-low density
young-old no craters-lots rock and iron-rock and ice |
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Saturn distinguishing features
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extensive ring system
roche limit prevents accretion of particles |
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Composition and Structure
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small rocky core, liquid ice layer, thin layer of liquid metallic hydrogen
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Titan
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half rock, half ice moon, thick atmosphere
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Roche limit
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prevents accretion
tidal forces=grav. forces between particles |
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Uranus distinguishing features
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perpendicular to ecliptic
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Structure and composition
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rocky core, salt water layer, liquid h2 and he layer
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Miranda
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Moon with chaotic terrain-smashed and reassembled
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Ring system
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thin
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Neptune distinguishing features
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great dark spot that vanished
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Composition and structure
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rocky core, salt water, liquid h2 and he layers
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Triton
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moon with retrograde motion and young surface
nitrogen geysers |
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Rings
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Thin and clumpy
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Pluto best observations
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Hubble telescope
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Charon
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moon, rotates in 6.4 days, always faces the same way
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Controversy
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KBO object or planet?
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