The Solar System
This is the age of our solar system.
~4.6 billion years ago
These are the three types of meteorites
Stony, Iron, & Stony-Iron
This is what drives plate tectonics
Convection in the Mantle
This term describes the breaking down and moving of rocks.
Erosion
These are the three types of impact craters
Simple (Bowl-shaped), Complex (Hill), and Multi-Ring
This is the term for the gradual piece-by-piece build up of a planetary body.
Accretion
Some stony meteorites are undifferentiated, meaning this
They have not undergone any process, like melting, that segregates elements because of their chemical properties
These are major contributors of the water vapor in Earth's atmosphere.
Volcanoes
These are the steps of the hydrologic cycle and what drives the cycle.
Evaporation, Condensation, Precipitation, Transpiration, & Runoff. The Sun!
These are the two major regions of the surface of the moon & their characteristics.
Maria (Seas): the relatively low, smooth, dark areas and Highlands/Terrae (Land): the densely cratered, rugged highlands
These are the major differences in the inner and outer planets (overall name, size, and composition).
Inner terrestrial planets (Mercury, Venus, Earth, Mars) are small and mostly made of silicate rocks & metals. The outer gaseous planets (Jupiter, Saturn, Uranus, Neptune) are large and consist of gaseous hydrogen, helium, and ice
Most meteorites are derived from these.
Asteroids.
These are the types of plate boundaries and activities associated with them
Divergent, Convergent (Subduction), and Transform. Volcanoes, Earthquakes, Mantle Plumes
This is why Earth's present atmosphere is different in composition than those of the other inner planets.
The present atmosphere contrasts sharply with those around other inner planets because it is poor in carbon dioxide, but rich in nitrogen and oxygen.
This is the composition of the Moon's Maria
Basaltic Lava
These are small icy bodies formed in the outer solar system. If their orbits become changed they may enter the inner solar system for a short time before they vaporize and break up
Comets
This is what meteorites are, therefore revealing information about the age and composition of solar system bodies.
Samples of a variety of bodies in the inner solar system. Many meteorites have been relatively unaltered since the earliest stages of the solar system, and they preserve the chemical and mineralogic characteristics of such ancient materials and of the processes that shaped them
This is how size of a planet impacts its heat.
Larger planets stay volcanically active for longer than small ones do, since they retain their internal heat.
This is where maximum sediment load occurs
In large rivers that drain a mountainous topography (fast moving) in a humid climate
These are factors that control the size of an impact crater.
Velocity, mass, density, gravity of impact planet
This is the reason some planets have atmospheres, while others do not.
Volcanic outgassing from a warm planet's interior allows the planet to gravitationally capture these gases into an atmosphere. Planets that cooled faster no longer have volcanic activity. Planet size, composition, and nature of internal and external heat sources impact this.
Over 95% of meteorites seen to have fallen onto Earth are these.
Stony Meteorites
These are all of Earth's interior layers, with their state of matter and composition.
Iron-rich core (solid inner core, liquid outer core), a thick mantle of iron- and magnesium-rich silicates (with a ductile/elastic layer), and a rigid crust of silica-rich rocks
This is how the number of tributaries connects to climate.
Networks of tributaries are expressions of the fact that the main source of water in Earth's rivers is from rain and surface runoff. In wetter climates, there are more tributaries.
This is the giant impact hypothesis.
Earth collided with a Mars-sized protoplanet about 4.5 billion years ago and some of the ejected debris from the impact event re-accreted to form the Moon.