Chapter 9. ASTRONOMY 202 Spring 2007: Solar System Exploration. Class 26: Planetary Geology [3/23/07] Announcements.

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1 ASTRONOMY 202 Spring 2007: Solar System Exploration Instructor: Dr. David Alexander Web-site: Class 26: Planetary Geology [3/23/07] Announcements Planetary Geology Planetary Surfaces Planet Interiors: Terrestrial Planets Chapter 9 Structure of the Interior Internal Heat The Mantle and Lithosphere Planetary Core and Magnetic Fields Now Playing: Continental Drift Rolling Stones

2 Announcements Web Project Window is open to choose web project window closes March 26 See class web-site for details and some news sites - science.nasa.gov is a good one for solar system Observing Observatory Open Night: Tonight 8:30pm Homework Homework #6 is available online and due Wed Mar 28

3 Planetary Geology Virtually all of the features we see in the terrestrial planets, moons, asteroids and comets today should be traceable to the properties they had at birth. Planetary Surfaces Seismic (tectonic) activity Volcanic activity Wind and rain erosion Cratering Water erosion

4 The interiors of terrestrial planets Most of the processes which shape the surfaces of planets are a result of what is going on inside them. Direct (e.g. seismic data) and indirect measurements (e.g. magnetic field data) show that surface rocks of all the terrestrial worlds are much less dense than the world as a whole: The interiors are denser

5 Layering by density: three basic layers Interior structure CORE MANTLE CRUST Nickel and Iron at high density Rocky material (e.g. minerals containing Silicon and Oxygen) surrounds core Lowest density rock (e.g. granite, basalt) forms thin crust

6 Earth s core The Earth s metallic core consists of a solid inner core and a molten (liquid) outer core. The distribution of the various materials in a terrestrial planet s interior results from a combination of temperature, density variations. In particular, the process of differentiation, where gravity orders the material by their density results in the layered structure of planetary interiors. The layering tells us that the planets were essentially liquid at one time for differentiation to work.

7 Layering by strength: the Lithosphere Interior structure The strength of the rock making up a planet s interior plays an important part in its geology. The Lithosphere encompasses the crust and part of the mantle and is defined by the strength of the rock rather than the density.

8 Layering by strength: the Lithosphere Interior structure The strength of the rock making up a planet s interior plays an important part in its geology. The Lithosphere encompasses the crust and part of the mantle and is defined by the strength of the rock rather than the density. Gravity will make any rocky object more than about 500 km in diameter into a sphere within about 1 billion years. The strength of a rock depends upon: composition temperature surrounding pressure - different molecular bonds - weakens bonds - strengthens bonds Earth and Venus have very thin lithospheres while the lithospheres of Mars, Mercury and the Moon include most or all of their mantles.

9 Internal Heat The different geology of the terrestrial worlds is strongly governed by their differences in internal heat. Main ways to heat a planet: Accretion Heat generated at formation Differentiation Re-distributes heat within planet Radioactive Decay Conversion of mass-energy to heat Radioactive decay is the only source of heat acting at the present time. Planets cool by emitting thermal radiation (as infrared radiation) with the rate of cooling being determined by their size (surface area to volume ratio).

10 Mantle Convection Relationship between internal heat and geological activity is the ability of rock to move within the mantle. Main ways to move energy in a planet: Convection Hot solid material expands and rises Cool material contracts and falls Conduction Transfer of heat through particles Radiation Thermal energy of surface radiates into space Rock strength (lithosphere) governs convection versus conduction Mantle convection is closely tied to lithosphere thickness.

11 Magnetic Fields Molten metals in the outer core of a planet can generate a magnetic field. Three basic requirements for a planet to have a magnetic field An interior region of electrically conducting fluid such as molten metal Convection in that layer of fluid At least moderately rapid rotation Earth is the only terrestrial planet with a strong magnetic field. The presence or lack of a magnetic field provides important clues to a planet s interior structure. Moon: no metals or solid core Mars: solidification of core Venus: slow rotation or little convection Mercury: has weak field despite being small and slow!

12 Shaping the surface of a planet The Four Basic Geological Processes Impact Cratering Formed by collisions of asteroids or comets with planet Volcanism Eruption of molten rock (lava) from planet s interior Tectonics Disruption of surface by internal stresses Erosion Wind, water, ice deformations of surface features

13 Impact Cratering Impacting objects typically hit a planet s surface at 30,000 to 250,000 km/hr. Craters are generally 10 times wider than the impacting object and about 10-20% as deep as they are wide. Crater is the Greek word for cup.

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