Interiors of Worlds and Heat loss Differentiation -materials

Interiors of Worlds and Heat loss Differentiation -materials

Interiors of Worlds and Heat loss Differentiation -materials separate into layers by gravity How do we learn about planetary interiors?

Measure moment of inertia & average density Observe seismic events Study planetary magnetic fields Interior of our planet gaseous atmosphere (lowest density)

Interior of Terrestrial Worlds Interiors: Gas Giant v.s Terrestrial Interior of Gas Giant Worlds The magnetic fields of gas giants indicate

that there are large amounts of circulating, electricallyconducting materials. Metallic hydrogen or water

Which of the following layers of a planet is not characterized by its density? A.core B.mantle C.lithosphere D.crust E.none of the above

2014 Pearson Education, Inc. Heat loss Planets gain their initial internal heat energy when

they first form Planet spend the rest of their lives losing internal energy to space 3 Types of Heat loss Conduction -atoms vibrate strongly causing atoms next them to pick up energy

Convection- heat causes fluids to move, the hot fluid rises, the cold fluid sinks. Radiation- photons of electromagnetic light carry energy away from the object Which Forms of Heat Loss Work Where?

All worlds conduct inside. All worlds radiate out to space (the only heat transfer that works in a vacuum!). Larger worlds convect inside. Largest worlds convect and radiate inside. (wavelength of radiation depends on world mass)

Solid Convection Causing Volcanism Solid convection causing movement, but no crustal break-up Solid convection causing crustal break-up (Earth only)

How does an object's rate of cooling vary with size? A. A larger object cools more slowly than a smaller object. B. A smaller object cools more slowly than a larger object. C. Size has no effect on an object's rate of cooling.

2014 Pearson Education, Inc. Geologic Processes Geological Processes Tectonics Rocks bend and break (folding and faulting).

Volcanism Materials melt, explode and freeze. Erosion and surface processes Surfaces flatten out: mountains crumble and holes are filled in.

Mass wasting (gravity action) Wind action Water action Impact Cratering (external)

Bodies from space hit the ground, making a hole. Tectonics -Folding When rocks are squashed they will compress and bend away from the direction of maximum pressure Tectonics -Faulting

1. Extension Faults -crust moves apart, makes a larger area. 1. Compression Faults -crust moves together, makes smaller area. 1. Strike-slip Faults -crust moves sideways, no gain or loss of area

What is true of convection that stresses a planet's crust? A. Mountains may form where the crust is pushed together. B. Cracks and valleys may form where the crust is pulled apart. C. Convection has no effect on a planet's crust.

D. A and B 2014 Pearson Education, Inc. Volcanism Materials melt, erupt and explode, then freeze and coat the surface Generic Volcano Structure

Volcanic Processes Rocks melt and explode. 2 components: lava, gasses Lavas - variable viscosity,depending on chemistry Low viscosity (runny lava)

range of viscosity (gooey, sticky lava) Low gas content Result: Low broad shapes shapes Volcanic

Shield Floods Volcanoes High viscosity High gas Result:

range of volcanoes Cinder cones Tall cone Stratovolcanoes

Volcanic Floods -VERY low Viscosity Hawaiian Effusive eruption Olympus Mons Martian Shield Volcano Note the broad shield

shape and the central cauldera Volcanic Processes Rocks melt and explode. 2 components: lava, gasses Lavas - variable viscosity,depending on chemistry Low viscosity

(runny lava) range of viscosity (gooey, sticky lava) Low gas content Result: Low broad shapes

shapes Volcanic Shield Floods Volcanoes High viscosity

High gas Result: range of volcanoes Cinder cones Tall cone

Stratovolcanoes Explosive Stratovolcanos Occur only on Earth a product of plate tectonics Alternative Materials

carbonatites, East Africa, Earth Water eruption plume, Enceladus sulfur volcanoes,

Io Erosion and Surface Processes Gravity pulls everything into a smooth sphere. Thus, surfaces flatten out: mountains crumble and holes are filled in. The processes that carry out erosion each show characteristic patterns that we can see on Earth and

on different worlds: Mass wasting (gravity action)- land slides Wind action- sand dunes, wind streaks

Water action- river channels, ocean shores, glacial erosion Sand Dunes in the Sahara (imaged by the Space Shuttle)

Ice/tar dunes on Titan Water Channels on Mars Ethane Channels on Titan Impact Cratering Bodies from space hit the ground, making a hole.

(the only external process -it comes to the planet from the outside) The size of the hole depends on the energy of the impact. A small, slow-moving, ice-ball makes a small hole. A massive, fast moving, rock makes a large hole.

Imbrium Basin Moon Crater Dating Solar System debris falls onto planets at a regular rate, making craters. The number of holes on a surface is a measure of how long it has been exposed to impacts.

Impact craters can be destroyed by the three internal processes (tectonics, volcanism, erosion) Surfaces with few craters have active processes destroying the craters. (called YOUNG surfaces) Surfaces with lots of craters have no active processes & are undisturbed. (OLD surfaces) Which Surface is Older?

B A Which World is More Active? (Be able to explain your choice) Earth

Moon Planetary Atmospheres Atmospheric Basics Our goals for learning What is an atmosphere?

How do you obtain an atmosphere? What is an atmosphere? An atmosphere is a layer of gas that surrounds a world How do you obtain an atmosphere? Gain volatiles by comet impacts

outgassing during differentiation Ongoing outgassing by volcanoes Keeping an Atmosphere Atmosphere is kept by the worlds gravity and temperatures

Low mass (small) worlds = low gravity = little atm. High mass(large) worlds = high gravity = thick atm. Low temperatures = slow gases = more atm. High temperatures =excited gases = atm.loss

Gravity and pressure Air pressure depends on how much weight of gas is there ie. The atmospheric thickness. What have we learned? What is an atmosphere? A layer of gas that surrounds a world

How do you obtain an atmosphere? comet impacts plus outgassing by differentiation, or volcanoes. How much atmosphere is retained depends on the worlds gravity and temperatures Atmospheric Processes 1 Our goals for learning

What are the key processes? What creates wind and weather? How does the greenhouse effect warm a planet? Atmospheric Processes Atmospheric circulation (convection) Convection cells move gas from equator to pole and

back. Coriolis Effect Gas dragged sideways by the rotation rate of the world. Greenhouse Effect Infrared energy is re-reflected back to the ground by

CO2 Air Movement Gas molecules move from high density to lower density Atmospheric Pressure Gas pressure

depends on both density and temperature. Adding air molecules increases the pressure in a

balloon. Heating the air also increases the pressure. (molecules more energetic)

Atmospheric Circulation (convection) Heated air rises at equator Maximum Sun warming

Cooler air descends at poles Coriolis Effect Coriolis Effect breaks up Global Circulation On Earth the large

circulation cell breaks up into 3 smaller ones, moving diagonally Other worlds have more or fewer circulation cells depending on their rotation rate

Coriolis Effect Winds blow N or S Venus Winds are diagonal

Earth Mars Winds blow W or E Jupiter, Saturn Neptune, Uranus(?) Greenhouse Effect

If there was no greenhouse effect, Earth... A. would be warmer than it is today. B. would have a thicker atmosphere. C. would be colder than freezing. D. would have no protection from ultraviolet radiation.

2014 Pearson Education, Inc. What have we learned? What creates wind and weather? Atmospheric heating and Coriolis effect. Solar warming creates convection cells. The coriolis effect drags winds sideways and breaks up

the cells The faster a planet spins, the more E-W gas movement there is How does the greenhouse effect warm a planet? Atmospheric molecules allow visible sunlight to warm a planets surface but absorb infrared photons, trapping the heat.

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