10. Terrestrial Planets: Evolution - University of Hawai»i
Transcript of 10. Terrestrial Planets: Evolution - University of Hawai»i
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Astronomy 241: Foundations of Astrophysics I
10. Terrestrial Planets: Evolution
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Internal Structure
Earth’s Interior & Plate Tectonics
Inner core (solid)Iron/Nickel/Cobalt
Outer core (liquid)Fe/Ni/Co & O/S?
Lower mantle (plastic)Rock (Si/Mg/O/Al/...)
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Evolutionary History: Deep Similarities
Terrestrial planets differentiated: high-density metal sank downward, while low-density rock floated upward.
To differentiate, the planets must have melted completely.
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Many CratersSmooth Plains
High Cliffs
Volcanos“Continents”Few Craters
VolcanosContinents!
Oceans
Many CratersHighlands
Smooth Plains
VolcanosSome Craters
Riverbeds?
Evolutionary HistoryHow did this variety arise?
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Evolutionary History: Size Makes a Difference
Large planets stay hot — why?
More volume per unit of surface.
More heat outflow through unit of surface.
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Evolutionary History: Cooling Off
Smaller planets have cooled more, and therefore are solid to greater depths.
Near-solid region is called the lithosphere.
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The Age of the Solar System
Radioactive elements decay into stable ones; e.g.,
(Potassium-40) (Argon-40) (positron)
40K → 40Ar + e+
The rate of decay is fixedby the element’s half-life, the time for 50% to decay; for 40K, this time is 1.25 Gyr (1 Gyr = 1 billion years).
Rocks contain no 40Ar when they form; by measuring the ratio of 40Ar to 40K, the rock’s age can be found.
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The Cartoon History of the Universe
The Age of the Solar System:Dating Rocks
• The oldest Earth rocks are ~3.8 Gyr old.
• The oldest Moon rocks are ~4.4 Gyr old.
• The oldest meteorites are 4.55 Gyr old; this is how long ago minerals started condensing in the disk.
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The Moon & Mercury
Both exhibit craters and smooth plains.
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Formation of the Moon by Giant Impact
Mars-sized planet (Thea) hits Earth about 4.5 Gyr ago.
This explains why Moon is poor in metals and volatiles.
Moon-forming impact
Moon forms from debris:
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Impact Cratering
• occurs on any body with a solid surface
• impact vaporizes projectile and comparable mass of target
• expanding vapor blasts material in all directions ⇒ circular crater
• craters typically 10 times diameter of projectile
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Crater Structure
Impact CrateringImpact Cratering
Small impacts produce simple bowl-shaped craters.
Large impacts produce craters with terraced rims and central peaks.
Impact Cratering
Impact Cratering
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Impacts: Formation of Lava Plains
4 Gyr ago, a heavily cratered surface. A few 100 Myr later, lava fills crater.A giant impact creates a huge crater.
The smooth lava plains of the Moon and Mercury are relics of impacts during “late heavy bombardment”.
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Impact Cratering: Late Heavy Bombardment
Time (Gyr ago) A Cool Early Earth
Evidence from Moon rocks suggests a peak in cratering rate about 3.8 to 4 Gyr ago.
This would have affected other planets as well.
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Mercury (compared to the Moon)
• Fewer craters — more buried by lava floods.
• Giant scarps (cliffs) — tectonic relic of global contraction.
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Internal Structure: Mantle Convection
Heat is carried by convection — slow circulation of semi-solid rock.
Convective Heat Transfer
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Mantle Convection
Internal Structure: Convection Simulation
Cold Downwellings Warm Upwellings
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Mantle Convection
Internal Structure: Convection Simulation
Cold Downwellings Warm Upwellings
Elapsed time: about 200 Myr.
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Mars: Dead or Just Chill?
Normal weather Global dust storm
Polar cap
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Mars: Surface Topography
Flat Topography Map of Mars
Cratered Highlands
Smooth Lowlands
Hellas
Tharsis Bulge
Olympus Mons
Valles Marineris
Evidence for a complex and varied geological history.
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Olympus Mons
Olympus Mons:hot-spot vulcanism
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Valles Marineris:tectonic stresses
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Meandering Riverbed?
Crater counts suggest an age of 2 to 3 Gyr.
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Evidence for Surface Water in Mars’s Past
Layered (sedimentary?) rock in eroded crater (right).
Surface feature resembling sedimentary rock (below).
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Water on Mars Today
Water on Mars
The North and South polar caps contain enough water to make an ocean 15 m deep . . .
More water may exist as permafrost elsewhere on the planet.
Liquid water cannot exist on surface under present conditions — it evaporates due to low pressure.
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Water on Mars
Water on Ancient Mars
Mars had a more massive CO2-rich atmosphere in the distant past.
The greenhouse effect probably warmed the planet above freezing.
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Venus: Just Passing By
The surface is hidden by thick clouds . . .
Venus Unveiled
but can be mapped by radar.
Venus: a Greenhouse Planet
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Impact crater (rare)
Shield volcanos Lava domes
“Corona” (mantle plume)
Fractured crust (tectonic)
Venus: Surface Features
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Venus: Surface Features
• Craters are rare because entire surface was “repaved” 500 — 750 Myr ago.
• Volcanic features are found everywhere, indicating ongoing volcanic activity.
• Tectonic features are unlike those on Earth; no plates!
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No Magnetic Field
yes — strong! none — why not?
not now; too cold?
weak; slow spin
none; cold
Thick, dry lithosphere traps heat inside.
Core can’t cool ⇒ no convection.
Heat build-up triggers global “repaving” events.
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Barringer Meteor Crater, Arizona
Manicouagan, Quebec, Canada
Impact Craterson Earth
Terrestrial Impact Craters
Impact melt breccia, Chicxulub
1.2 km
Age: 49,000 yr
70 km
Age: 212 Myr
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Volcanoeson Earth
Mauna Loa Volcano, HawaiiWikipedia: Mount Fuji
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Erosionon Earth
Grand Canyon, Arizona
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Plate Tectonics
Earth’s crust is a collection of slowly-moving plates.
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Plate Tectonics: Earthquakes
The plate boundaries are often sites of earthquakes.
Evidence for Plate Tectonics
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Wikipedia: Plate Tectonics
Plate Tectonics
Mantle convection drives plate motion.
Plates are formed at ocean ridges and continental rifts, and destroyed in subduction zones.
Plates float on denser mantle material.
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Evidence for Plate Tectonics
Plate Tectonics: Age of Sea-Floor
Ages confirm picture of plate formation at ocean ridges.
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Breakup of Pangaea
Plate Tectonics: Continental Drift
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Atmosphere
Venus Earth Mars
Venus Earth MarsCO2
N2
O2
Arpressure
96.5% 0.038% 95.3%3.5% 78% 2.7%
21%0.93% 1.6%
92 1.0 0.006
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Secondary Atmospheres
Volcanos releaseCO2, H2O, etc
Impacts deliverH2O, CO, etc
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Venus: Atmosphere
— 96% CO2; traces of N2, SO2, H2SO4, etc.
Properties:
— about 90 times mass of Earth’s atmosphere!
Why no H2O? (should be released by volcanos)
— Solar UV radiation breaks up H2O
— Hydrogen is stripped away by solar wind
— Oxygen reacts with surface rocks
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Wikipedia: Oxygen Cycle
Earth: O2 Cycle
Biological processes are the key sources and sinks of O2:6 CO2 + 6 H2O + energy ⇆ C6H12O6 + 6 O2
Most O2 is underground, but exchange between atmosphere and biosphere is the major pathway.
Amount of O2 is kept fairly constant by competition between sources and sinks.
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Earth: CO2 Cycle
Carbon and oxygen cycle together over short times.
Over longer times, carbon cycles deep underground.
CO2 in airfalls as
acid rain
dissolves minerals
forms carbonates
subducted underground
returned by volcanos
This regulates Earth’s climate (very slowly):
too ⇒ rain ⇒ CO2 in air ⇒ greenhousehotcold
moreless
lessmore
weakerstronger
Plate tectonics is necessary to return buried carbon!
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Climate Cycles
Time (kyr)Wikipedia: Milankovitch Cycles
Small regular changes in Earth’s orbit and tilt vary the amount of sunlight the northern continents receive.
This triggers an ice-age every 105 yr (roughly).
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CO2 and Ice Ages
1. During an ice age, surface ice covers the oceans.
2. CO2 from volcanic outgassing builds up.
3. High CO2 produces rapid warming, ending ice age.
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Climate and CO2
CO2 concentration and temperature track each other.
Peaks in temperature match peaks in CO2
Now, humans activity is increasing CO2 concentration.