The Terrestrial Planets Astronomy 311 Professor Lee Carkner Lecture 9.
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Transcript of The Terrestrial Planets Astronomy 311 Professor Lee Carkner Lecture 9.
Where did the Earth come from?
a) It accreted from rocky planetesimalsb) It accreted from rocky and icy planetesimalsc) It rapidly condensed out of the solar nebulad) It was captured by the Sun’s gravitye) It was ejected from a collision of Jupiter and
Saturn
Why do we think the planet Jupiter formed quickly?
a) Samples from Jupiter indicate it is older than the other planets
b) It is mostly made of hydrogen gas which was only around in the early solar system
c) We see many Jupiter-type planets around very young stars
d) Jupiter’s orbit is right at the spot where the solar system was born
e) Jupiter has a very rapid rotation rate
Early Missions to the Inner Planets 1962 -- Mariner 2
Venus Fly-by
1964 -- Mariner 4 Mars Fly-by
1970 Venera 7 Venus lander first successful landing
on another planet
1973 Mariner 10 Venus/Mercury Fly-by
1975 Viking 1 and 2 Mars lander first successful landing
on Mars
Planetary Missions First wave of exploration from 1960-1979
Very large number of Soviet missions, most
were failures Venus: 15 successes, 31 missions
Smaller number of US missions, but higher success rate Mercury: 1 success, 1 mission Venus: 6 successes, 7 missions
We are now starting to see other countries get more involved with space exploration Most notably Japan and The European Union
Sources of Information for the Inner Planets
Mercury: Mariner 10 --
Venus: Soviet Venera landers -- surface conditions Magellan --
Mars: Viking, Pathfinder, Spirit, Opportunity --
Viking, Global Surveyor, Odyssey, Recon Orbiter -- maps of the surface
Inner Planet Facts
Mercury Diameter: 0.38 Mass: 0.06 Orbital Radius: 0.4
Venus Diameter: 0.95 Mass: 0.82 Orbital Radius: 0.7
Earth Diameter: 1 Mass: 1 Orbital Radius: 1
Mars Diameter: 0.53 Mass: 0.11 Orbital Radius: 1.5
Determining Planetary Properties
Mass
Distance Can find directly with radar
Diameter Can get from the angular diameter
and the distance
Determining Planetary Properties (cont.)
Average Density
Atmospheric composition take a spectrum of the atmosphere,
look for the spectral signature of elements
Scale Models
We want to make a scale model to try to understand astronomical distances
Need to find the scalescale = (real size) / (model size)
example: miles per inch or light years per cm
Once you have the scale you can find the model size for any real object
(model size) = (real size) / scale
The Planets That Weren’t There should have been 2 other inner
planets
A planet about the size of Mars may have hit the Earth a few billion years ago, the debris formed into the Moon
Jupiter’s gravity disrupted the planetesimals
between Mars and Jupiter so they never formed a planet
The Moon Most of our information comes from the
6 Apollo landings (11-17, excluding 13) Moon facts
Diameter: 0.27 Mass: 0.01 Orbital Radius (from Earth): 0.003
Moons of the Inner Planets Venus and Mercury have no moons Earth has one large moon
Mars has two moons, Phobos and Deimos
Inner planets may be too small to capture moons easily It is difficult to gravitationally capture something
Asteroids Millions of small bodies orbit the Sun, most
between Mars and Jupiter (the asteroid belt)
Our information comes from 2 sources:
Pieces of asteroids that have fallen to Earth
For example: NEAR orbiting Eros Hayabusa landing on Itokawa
Asteroid Facts Asteroids
Diameter: <0.14 Mass: <0.02 Orbital Radius: 2.8
Most have orbits within the asteroid belt (~2-3.5 AU)
Sizes of the Inner Planets Sizes relative to Earth
Earth: 1 (diameter = 13,000 km) Venus: 0.95 Mars: 0.53 Mercury: 0.38 Moon: 0.27 Asteroid: <0.01
All are small compared to the gas giants (Neptune is ~4 times the diameter of the Earth and ~64 times the volume)
Atmospheres
Mars Surface pressure = Composition = 95 % CO2, 3 % N (also water vapor,
oxygen) Venus:
Surface pressure = Composition = 96 % CO2, 4 % N (also sulfur
compounds such as sulfuric acid, H2SO4)
Atmospheres (cont.) Earth:
Surface pressure = Composition = 77 % N, 21 % O2 (also water
vapor, CO2, trace elements) Why are the atmospheres of Venus,
Mars and the Earth so different? The Earth can regulate its atmosphere
through the carbonate-silicate cycle, the other planets cannot
The Carbonate-Silicate Cycle
Water+
CO2
(rain)
Ocean
Carbonate + silicate(Sea floor rock)
CO2
Volcano
Atmosphere
Carbonate+ water(stream)
CO2 + silicate(subvectivemelting)
CO2 and Greenhouse Effect
Water washes CO2 out of atmosphere where it is eventually deposited as rock
CO2 is a greenhouse gas
More CO2 = higher temperature
CO2 and the Inner Planets Venus:
all the water boiled off and was disassociated
thick CO2 atmosphere and high temperatures
Mars: no way to get CO2 out of rocks
thin CO2 atmosphere and low temperatures
Earth:
mild temperature and atmosphere
Composition
Density of rock (silicates) ~3000 kg/m3
What makes up the difference? Iron
“Rocky” planets could also be called the “metal” planets
Composition (cont.)
Earthquake studies indicate that the Earth has a iron core Earth has a density gradient, heavier
materials near the center, lighter near the surface
We believe that the other inner planets have a similar structure
Summary Inner or Terrestrial region
4 planets (Mercury, Venus, Earth, Mars) 1 large moon (The Moon) thousands of asteroids
Information from 30 years of space missions Size
Earth and Venus about the same Mars, Mercury, the Moon, 1/2 -1/4 size of the
Earth Asteroids few km
Summary (cont.) Composition
silicate rock crust iron-silicate mantle iron core each planet has different proportions of each
Atmosphere Mercury, Moon, asteroids -- none Venus -- no water means CO2 is in atmosphere
Mars -- no plate tectonics means CO2 is in rocks Earth -- carbonate-silicate cycle balances greenhouse
effect