© 2005 pearson education inc., publishing as addison-wesley planetary atmospheres gases surrounding...
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© 2005 Pearson Education Inc., publishing as Addison-Wesley
Planetary Atmospheres
Gases SurroundingEarth and the Other Terrestrial Worlds
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Homework due Friday (as always).
Telescope Opportunity: View Saturn, Orion nebula, Venus, Any Other Celestial Object Sketch two of them.
TALC: every wed 7-9pm
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Planetary Atmospheres
The layer of gas surroundingEarth and the Other Terrestrial Worlds
Breathe: N2 O2 CO2
• Oxygen we breathe• Shields UV photons• Protects us from meteorites• Traps heat in: Greenhouse Effect
• Earth’s Atmosphere Unique in Solar System: Only one with oxygen. Luck . . . ?
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Earth’s Atmosphere
• 78% NITROGEN (N2)
• 21% OXYGEN (O2)
• 0.04% CARBON DIOXIDE (CO2)
• ~1% ARGON (Ar)
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• Produced by plants during photosynthesis• Necessary for breathing by animals.• Arrived 3.5 billion years ago- algae bacteria
• Water vapor (H2O)• Carbon monoxide (CO)• Neon (Ne)• Oxides of nitrogen• Methane (CH4)• Krypton (Kr)
Concentrations are a fewparts per million (ppm)
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O O
O C O
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Carbon Dioxide:in our atmosphere is
Increasing rapidly
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Worldwide CO2 EmissionBy fuel type: 1970 - 2020
CO2 Causes Global Warming:Stay tuned . . .
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Burning coal
gasoline
Natural gas
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General Origin of Terrestrial Atmospheres
• Venus, Earth, & Mars received their atmospheres
through volcanic outgassing.• H2O, CO2, N2, H2S, SO2
• On Earth:• CO2 on Earth dissolves in oceans and goes into carbonate rocks like
limestone (= calcium carbonate, Ca CO3.)
• Made possible because H2O could exist in liquid state
• N2 was left as the dominant gas;
• O2 from photosynthesis
• Mars and Venus: CO2 is dominant gas
• Mars: lost much of its atmosphere through impacts• less massive planet, lower escape velocity
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Origin of Earth’s Atmosphere
Volcanic Outgassing:H2O, CO2, N2, H2S . . .
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Origin of Atmospheric Gas:Volcanic Outgassing
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What about Oxygen? Where did it dome from?
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Origin of Oxygen on Earth:Plants
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Fossilized remains of blue-green algae
Appears 3 billion
years ago.
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cyanosarcina
Shark’s Bay (Western Australia):Colonies of microbes: Stramatolite (blue-green algae)
Evidence of Oxygen actually
produced?
(radioactive age dating)
Banded-iron Formation
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Octopus spring (Yellowstone)Photosynthetic Blue-green algae mats
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Gain/Loss Processes of Atmospheric GasGain/Loss Processes of Atmospheric Gas
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Comparing Terrestrial Atmospheres
Mercury: none Venus: CO2 massive atm. Earth: modest
Mars: CO2 1% of Earth’s pressure
Moon: None
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What is an Atmosphere ?
• A layer of gas which surrounds a world • Usually very thin compared to planet radius• Temperature: Measure of Avg. speed of molecules• Pressure: Force per area caused by atoms & molecules
colliding with walls or each other.• heating a gas in a confined space increases pressure
• number of collisions increase
• unit of measure: 1 bar = 14.7 lbs/inch2
Earth’s atmospheric pressure at sea level
• Pressure balances gravity in an atmosphere.
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Why doesn’t the atmosphere fall down due to gravity?
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Atmospheric Pressure:Balances gravity
• Upward pressure
supports air against
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Atmosphere
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Planetary Energy Balance• Planet receives Solar energy • Surface Warms.• Thermal emission in infrared light increases until the energy emitted equals solar energy received: ===> stable
temperature
What if Earth getstoo hot ? Can itcorrect the temperatureBack to normal?
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Effects of an Atmosphere on a Planet
• Greenhouse effect• makes the planetary surface warmer than it would be otherwise
• Scattering and absorption of light• absorb high-energy radiation from the Sun• scattering of optical light brightens the daytime sky
• Creates pressure• can allow water to exist as a liquid (at the right temperature)
• Creates wind and weather• promotes erosion of the planetary surface
• Creates auroras• interaction with the Solar wind when magnetic fields are present
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The Greenhouse Effect: Planetary Temperature
• What is the greenhouse effect?
• Is it good, bad, or both . . .
• How would planets be different without the greenhouse effect?
• Compare the greenhouse effect on
Venus, Earth, and Mars.
Questions:
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The Greenhouse Effect
• Visible Sunlight passes through a planet’s atmosphere.
• Some of this light is absorbed by the planet’s surface.
• Planet warms. Emits its own light: “thermal radiation”, as infrared (IR) light - back out to space.
• IR light is “trapped” by the IR light is “trapped” by the atmosphere.atmosphere.• Its return to space is slowed
• Causes the temperature to be higher than if there were no atmosphere at all.
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Greenhouse Gases
• Key to Greenhouse Effect…gases which absorb IR light effectively: • water [H2O]
• carbon dioxide [CO2]
• methane [CH4]
• These are molecules which rotate and vibrate easily.• they re-emit IR light in a random
direction
• The more greenhouse gases which are present, the greater the amount of surface warming.
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What Determines a Planet’s Surface TemperatureWhat Determines a Planet’s Surface Temperature?
• Greenhouse Effect cannot change incoming Sunlight, so it cannot change the total energy returned to space.• it increases the energy (heat) trapped in lower atmosphere• it works like a blanket
• In the absence of the Greenhouse Effect, what would determine a planet’s surface temperature?• the planet's distance from the Sun• the planet’s overall reflectivity, “albedo” (fraction reflected)
• the higher the albedo, the less light absorbed, planet cooler
• Earth’s average temperature would beEarth’s average temperature would be ––17º C (–1º F) without the Greenhouse Effect !17º C (–1º F) without the Greenhouse Effect !
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What Determines a Planet’s Surface Temperature?
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Greenhouse Effect on the PlanetsGreenhouse Effect on the Planets
• Greenhouse Effect warms Venus, Earth, & Mars• on Venus: it is very strong
• on Earth: it is moderate
• on Mars: it is weak
• avg. temp. on Venus & Earth would be freezing without it
albedo
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Atmosphere: Layered Structure
• Basic structure of Earth’s atmosphere.
• Heating from causes atmospheric structure
• Contrast Venus, Earth, and Mars.
• Magnetosphere?
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Earth’s Atmosphere
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Structure of Earth’s AtmosphereStructure of Earth’s Atmosphere• Pressure & density of atmosphere decrease with altitude• Temperature increases and decreasesvaries with altitude
• temperature domains define the major atmospheric layers
• exosphere
• low density; fades into space
• thermosphere
• temp begins to rise at the top
• stratosphere
• rise and fall of temp
• troposphere
• layer closest to surface
• temp drops with altitude
Ozone Layer (absorbs UV)
(mesosphere)
Troposphere
Stratosphere
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Atmospheres Interact with Light• X rays
• ionize atoms & molecules
• dissociate molecules
• absorbed by almost all gases
• Ultraviolet (UV)• dissociate some molecules
• absorbed well by O3 & H2O
• Visible (V)• passes right through gases
• some photons are scattered
• Infrared (IR)• absorbed by greenhouse gases
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Reasons for Atmospheric Structure • Absorption of sunlight energyAbsorption of sunlight energy causes layering structure.
• Troposphere• absorbs IR photons from the surface
• temperature drops with altitude
• hot air rises and high gas density causes storms (convection)
• StratosphereStratosphere• lies above the greenhouse gases (no IR absorption)
• absorbs heat via Solar UV photons which dissociate ozone (O3)
• UV penetrates only top layer; hotter air is above colder air
• no convection or weather; the atmosphere is stratified
• ThermosphereThermosphere• absorbs heat via Solar X-rays which ionizes all gases
• contains ionosphere, which reflects back human radio signals
• Exosphere• hottest layer; gas extremely rarified; provides noticeable drag on satellites
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Structure of Terrestrial Planet Atmospheres
• Mars, Venus, Earth all• have warm tropospheres
(and greenhouse gases)• have warm thermospheres
which absorb Solar X rays
• Only Earth has• a warm stratosphere • an UV-absorbing gas (O3)
• All three planets have warmer surface temps due to greenhouse effect
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Magnetospheres
• The Sun ejects a stream of charged particles, called the solar wind.• it is mostly electrons, protons, and Helium nuclei
• Earth’s magnetic field attracts and diverts these charged particles to its magnetic poles.• the particles spiral along magnetic field lines and emit light
• this causes the aurora (aka northern & southern lights)
• this protective “bubble” is called the magnetosphere
• Other terrestrial worlds have no strong magnetic fields• solar wind particles impact the exospheres of Venus & Mars
• solar wind particles impact the surfaces of Mercury & Moon
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Earth’s Magnetosphere
SolarWind:Electrons, protons, helium nuclei
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What are Weather and ClimateWhat are Weather and Climate?
• These are Earth’s global wind patterns or circulation• local weather systems move along
with them
• weather moves from W to E at mid-latitudes in N hemisphere
• Two factors cause these patterns• atmospheric heating
• planetary rotation
Weather – short-term changes in wind, clouds, temperature, and pressure in an atmosphere at a given location
Climate – long-term average of the weather at a given location
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Global Wind PatternsGlobal Wind Patterns• Air heated more at equator
• warm air rises at equator; heads for poles
• cold air moves towards equator along the surface
• Two circulation cells are created in each hemisphere
• Cells of air do not go directly from pole to equator; air circulation is diverted by…
• Coriolis effect• moving objects veer right on a
surface rotating counterclockwise• moving objects veer left on a
surface rotating clockwise
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Global Wind PatternsGlobal Wind Patterns• On Earth, the Coriolis effect breaks each circulation
cell into three separate cells• winds move either W to E or E to W
• Coriolis effect not strong on Mars & Venus• Mars is too small
• Venus rotates too slowly
• In thick Venusian atmosphere, the pole-to-equator circulation cells distribute heat efficiently
• surface temperature is uniform all over the planet
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Clouds, Rain and Snow
• Clouds strongly affect the surface conditions of a planet• they increase its albedo, thus reflecting away more sunlight• they provide rain and snow, which causes erosion
• Formation of rain and snow:
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Four Major Factors that affect Long-term Climate Change
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Gain/Loss Processes of Atmospheric Gas
• Unlike the Jovian planets, the terrestrials were too small to capture significant gas from the Solar nebula.• what gas they did capture was H & He, and it escaped
• present-day atmospheres must have formed at a later time
• Sources of atmospheric gas:• outgassing – release of gas trapped in interior rock by
volcanism
• evaporation/sublimation – surface liquids or ices turn to gas when heated
• bombardment – micrometeorites, Solar wind particles, or high-energy photons blast atoms/molecules out of surface rock
• occurs only if the planet has no substantial atmosphere already
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Gain/Loss Processes of Atmospheric Gas
• Ways to lose atmospheric gas:• condensation – gas turns into liquids or ices on the surface
when cooled
• chemical reactions – gas is bound into surface rocks or liquids
• stripping – gas is knocked out of the upper atmosphere by Solar wind particles
• impacts – a comet/asteroid collision with a planet can blast atmospheric gas into space
• thermal escape – lightweight gas molecules are lost to space when they achieve escape velocity
gas is lost forever!
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Origin of the Terrestrial Atmospheres• Lack of magnetospheres on Venus & Mars made
stripping by the Solar wind significant.• further loss of atmosphere on Mars
• dissociation of H2O, H2 thermally escapes on Venus
• Gas and liquid/ice exchange occurs through condensation and evaporation/sublimation:• on Earth with H2O
• on Mars with CO2
• Since Mercury & the Moon have no substantial atmosphere, fast particles and high-energy photons reach their surfaces• bombardment creates a rarified exosphere
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11.6 The Climate Histories of Venus, Earth, and Mars
• Describe major, seasonal features of Martian weather today.
• Why did Mars’s early warm and wet period come to an end?
• Why is Venus so hot?• Could Venus ever have had oceans? • After studying Mars and Venus, why does
Earth’s atmosphere seem surprising?
Our goals for learning:
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Martian Weather Today
• Seasons on Mars are more extreme than on Earth• Mars’ orbit is more elliptical
• CO2 condenses & vaporizes at opposite poles• changes in atmospheric pressure drive pole-to-pole winds
• sometimes cause huge dust storms
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Mars’ Thin Atmosphere
• Martian sunset illustrates just how thin the Martian atmosphere is.
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Martian Weather: N Polar Ice Cap & Dust Storm
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Climate History of Mars
• More than 3 billion years ago, Mars must have had a thick CO2 atmosphere and a strong greenhouse effect.• the so-called “warm and wet period”
• Eventually CO2 was lost to space.• some gas was lost to impacts
• cooling interior meant loss of magnetic field
• Solar wind stripping removed gas
• Greenhouse effect weakened until Mars froze.
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© 2005 Pearson Education Inc., publishing as Addison-Wesley
Venusian Weather Today
• Venus has no seasons to speak of.• rotation axis is nearly 90º to the ecliptic plane
• Venus has little wind at its surface• rotates very slowly, so there is no Coriolis effect
• The surface temperature stays constant all over Venus.• thick atmosphere distributes heat via two large circulation cells
• There is no rain on the surface.• it is too hot and Venus has almost no H2O
• Venusian clouds contain sulfuric acid!• implies recent volcanic outgassing?
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© 2005 Pearson Education Inc., publishing as Addison-Wesley
Climate History of Venus• Venus should have outgassed as much H2O as Earth.
• Early on, when the Sun was dimmer, Venus may have had oceans of water
• Venus’ proximity to the Sun caused all H2O to evaporate.
• H2O caused runaway greenhouse effect
• surface heated to extreme temperature
• UV photons from Sun dissociate H2O; H2 escapes, O is stripped