Physical Science 101
Planet means _______________
Aug. 24, 2006, International Astronomical Union (IAU) formally defined a planet as:
Human Exploration - Apollo 11, 12, 14, 15, 16, 17
Planetary Probes (excluding Earth orbiting)
Mercury: Mariner, Messenger
Lunar: Pioneer, Luna, Ranger, Surveyor, Lunar Orbiter, PFS, Hiten, Hagoromo, Clementine, Lunar Prospector
Mars: Mars, Zond, Mariner, Cosmos, Viking, Phobos, Mars Observer, Mars Global Surveyor, Mars Pathfinder, Nozomi, Mars Climate Orbiter, Mars Polar Lander, Mars Odyssey, Mars Express, Spirit, Opportunity
Asteroids: NEAR, Hayabusa, Deep Space 1
Outer Planets: Pioneer, Voyager, Galileo, Cassini
Comets: Giotto, Stardust, CONTOUR, Rosetta
Additional information can be found at the Planetary Geology - Exploration page.
Differentiated interior: density layering
Atmosphere / Ocean
Processes which create: igneous and metamorphic material; surface landforms
Tectonics and Plate Tectonics
Magmatism and Volcanism
Core and Mantle Convection
Deformation and structural behavior of crustal material.
Heat from the core drives convection in the mantle.
Sources of Heat?
Mantle convection creates stress in the crust causing it to deform
Tectonic activity only occurs in planets with warm interiors.
Stress is any force which acts to deform rocks.
Heat from the core migrates towards the crust and causes mantle and crustal material to melt.
Molten or melted material is called ___________.
Magma is hot, therefore less dense than the surrounding material
What happens to the magma?
If the magma rises through the crust and reaches the surface:
Processes which erode and shape surface.
Major Factors of Planetary Erosion
Other Factors of Planetary Erosion
Critical erosion factors on Earth:
The mechanical and chemical destruction of the land (weathering) and the removal or transportation of material by flowing liquid (water), flowing or moving solids (ice, glaciers, impactors) or moving gas (wind).
The alteration of the surface of small bodies unprotected by an atmosphere.
Iron nanoparticles are formed by the evaporation of minerals during micrometeorite impacts or exposure of the surface to the solar wind
Iron nanoparticles then condense onto nearby mineral surfaces
Importance of this process:
Small craters (simple craters) are <16 km diameter; smooth bowl- or cone-shaped interiors (some with flat bottoms) - exterior deposits slope away from rim
Large craters (complex craters and basins) - roughly circular, terraced rims with a central peak or ring peak, surrounded by hummocky debris; >16 km diameter
The term applied to craters larger than 200 km is basin
Similar structure to large craters, but bigger
- roughly circular
- terraced rims with a central peak or ring peak
- surrounded by hummocky debris
- lava flows often fill the basin bottom
Cratering Process - Simple Craters
Cratering Process - Large Craters and Basins