ch11 note Zhang

Mercury, Venus and Mars: 

Mercury, Venus and Mars Chapter Eleven

Introduction To Modern Astronomy I:Solar System: 

ASTR 111 – 003 Fall 2007 Lecture 10 Nov. 05, 2007 Introducing Astronomy (chap. 1-6) Introduction To Modern Astronomy I: Solar System Planets and Moons (chap. 7-15) Sun and Life Highlights Chap. 16 & 28 Ch7: Comparative Planetology I Ch8: Comparative Planetology II Ch9: The Living Earth Ch10: Our Barren Moon Ch11: Mercury, Venus and Mars Ch12: Jupiter and Saturn Ch13: Satellites of Jupiter & Saturn Ch14: Uranus, Neptune and Beyond Ch15: Vagabonds of Solar System

Slide3: 

Mercury Data Moon-like

Slide4: 

Venus Data Covered by thick atmosphere

Slide5: 

Mars Data Earth-like, similar in day and season

Slide6: 

Viewing Mercury and Venus They are always close to the Sun in the sky Venus is brightest in the sky except Sun and Moon Mercury is also one of the brightest Mercury: a=0.38 AU, e=0.20 Venus: a=0.72 AU, e=0.007

Slide7: 

Viewing Mercury and Venus Greatest eastern elongation & Evening Star Planet appears after sunset, called “evening star” Greatest Western elongation & Morning Star Planet appears before sunrise, called “Morning star” Venus: 47°, ~ 3 hr Mercury: 28°, ~ 2 hr

Slide8: 

Opposition: the best Earth-based view of Mars The Earth-Mars distance can be as small as 0.37 AU Opposition occurs every 25 months, the synodic period Viewing Mars Mars: a=1.52 AU, e=0.093

Rotation of Planets: 

Rotation of Planets Mars P= ~ 1 day (23 h 23 m) P Known In 1666 Tilt: 25° Venus P= 243 days P not known till 1960! Tilt: 177° (retrograde) Mercury P= 59 days P not known till 1960! Tilt: 0.5° Why is difficult to observe rotation of Mercury and Venus?

Rotation of Mercury: 

Rotation speed is measured using Doppler effect with Radar Mercury has 3-to-2 spin-orbit coupling, with rotation period of 58.6 days and orbital period 87.9 day. It is in contrast to the expected synchronous rotation, or 1-to-1 spin-orbit coupling, e.g, Moon, which is caused by tidal force Rotation of Mercury Radar Measurement Using Doppler Effect. Arecibo Observatory in Puerto Rico

Rotation of Mercury: 

Explanation of Mercury’s 3-to-2 spin-orbit coupling Because of its high eccentric orbit (e=0.20). Tidal force tends to keep Mercury’s long axis point toward the Sun Because of the varying orbital speed, the pointing varies. The favorable pointing occurs only at the perihelion In one orbital period, Mercury spins 1.5 times. Rotation of Mercury Movie: 1-1 Movie: 3-2

Rotation of Venus: 

Rotation of Venus is peculiar Extremely slow:243 days (longer than orbital period 224 days) Retrograde rotation: opposite of direction of orbital motion All planets and satellites have prograde rotation except Venus, Uranus No good explanation on the retrograde motion??? Rotation of Venus

Mercury: 

Can we construct a consistent picture on the properties of the surface, interior and atmosphere of a planet (or moon), simply based on the size of the object? Small object: no atmosphere, no internal heat, no geological activity, old surface, no global magnetic field, e.g., Moon Large object: thick atmosphere, internal heat, geological activity, young surface, global magnetic field, e.g., Earth Mercury Mercury No atmosphere Surface is old, heavily cratered like the Moon No evidence of ongoing tectonics. These are consistent with its small size. Heavy cratered Mercury

Mercury: 

Scarp: long cliff on the surface As much as 3 km high and 20 to 500 km long Not produced by plate tectonics Caused by the shrinkage of Mercury’s crust as it cooled in the ancient time Mercury Scarp Movie: scarp formation

Mercury: 

Interior of Mercury: crust, mantle and core, like Earth Mercury’s core is relatively large The core is 75% of its diameter The earth’s core is 55% of its diameter the moon’s core is 20% of its diameter Mercury

Mercury: 

To account for Mercury’s large core and high iron content, one theory proposes that a collision with a planet-sized object stripped Mercury of most of rocky mantle. Mercury Surprising: Mercury has global magnetic field The old surface feature indicates no internal heat, thus not likely a liquid core It is an exception to the general rule No good explanation

Venus & Mars: Speculation: 

Venus was thought to be a tropical paradise Surface temperature 45° without greenhouse effect Actual surface temperature 460° due to strong greenhouse effect of its thick atmosphere Earth temperature is raised 33° due to greenhouse effect (from -19° to 14°) Mars was thought to have canals, plant life, even Martians Venus & Mars: Speculation Schiparelli’s drawing of Martian canals (1877) Lowell reported 160 canals by 1900 Scientists can be collectively wrong at one point of time

Venus & Mars: Surface: 

Tectonics: a study of the crust Earth plate tectonics: the crust is divided into several large pieces (~10); young surface Due to moderate internal heat Venus Flake tectonics: the crust breaks up into numerous flakes, producing small scale deformation and reshaping of the surface; young surface Due to relatively strong internal heat Mars Neither plate nor flake tectonics; thick & rigid crust; old surface Due to relatively weak internal heat Venus & Mars: Surface

Venus: Surface: 

The size implies that Venus retains sufficient heat inside. Small number of craters indicates that Venusian surface is about 500 million year old, indicating geological activity The surface of Venus is flat, only a few major highlands No long chain of mountain, inconsistent with plate tectonics Venus: Surface Topographic Map of Venus

Venus: Surface: 

Explanation: flake tectonics Convection currents in Venus’s interior are more rigorous than inside the Earth Strong convection prevents the formation of thick crust A thin crust undergoes wrinkling and flaking. Venus: Surface

Venus: Surface: 

Venus: Surface Plate Tectonics versus Flare Tectonics

Slide22: 

Surface in the south is heavily cratered, indicating an old surface and no recent geological activities Crustal dichotomy: Southern highlands ( 5 km higher) versus northern lowlands Surface in the north is smooth and free of craters, indicating relatively young Mars: Surface Topographic Map of Mars

Slide23: 

Mars has no ongoing geological activity. However, Mars had ancient geological activity, e.g, huge volcano mountains and deep rift valleys. Mars: Surface Mars Valles Marineris

Venus and Mars: Surface: 

Venus and Mars: Surface Volcanoes Earth: mostly extinct, some remain active Venus: probably like the Earth, only some active Mars: no active volcanoes, all extinct Volcanoes on Venus Volcanoes on Earth

Venus and Mars: Atmosphere: 

Venus and Mars: Atmosphere The Question: Why do Earth, Venus and Mars have dramatically different atmosphere? Even though the original atmospheres of the three planets were essentially the same, predominantly water vapor and carbon dioxide.

Venus and Mars: Atmosphere: 

Venus and Mars: Atmosphere Earth Pressure: 1 ATM (atmosphere) Temperature:14°C Cloud: H2O Venus Pressure: 90 ATM, High Temperature: 460°C Cloud: H2SO4 Mars Pressure: 0.006ATM Low Temperature: -23°C Cloud: CO2 & H2O

Venus: Atmosphere: 

Venus: Atmosphere Venus is the hottest planet, with a surface temperature of 460°C The high temperature is caused by extremely strong greenhouse effect, thanks to the presence of a large amount of CO2, which raises the surface temperature by more than 400°C Composition: Mostly carbon dioxide: 96.5% Remaining is Nitrogen: 3.5% Similar to Mars Venus has perpetual thick clouds The clouds have three layers from 48 km to 68 km Clouds mainly consist of droplets of concentrated sulfuric acid (H2SO4: highly corrosive).

Mars: Atmosphere: 

Mars: Atmosphere Mars is cold, average temperature -23°C Its atmosphere extremely thin, 0.006 ATM Greenhouse effect is very weak, due to the thin atmosphere, raising temperature by only 5°C (Earth 33°C, Venus 400°C). Composition: Mostly carbon dioxide: 95.3% Remaining is Nitrogen: 2.7% Similar to Venus

Mars: Atmosphere: 

Mars: Atmosphere Seasonal changes In the winter, the ice cap at polar regions grow, due to freezing-out of atmospheric carbon dioxide (forming dry ice). In the summer, it evaporates and the cap shrinks. Ice Cap Seasonal Change Frost of Freezing Carbon Dioxide

Mars: Atmosphere: 

Mars: Atmosphere Global dust storm: triggered by the flow of carbon dioxide evaporating from the polar ice cap with the coming of spring. Dust devil: each afternoon parcels of warm air rise from the heated surface and form whirlwinds A Martian Dust Storm A Martian Dust Devil

Evolution of Atmosphere: 

Evolution of Atmosphere The origin of atmosphere Outgassing of volcanoes: gases trapped in the rocks and but emitted through active volcanoes. The early atmospheres should be similar in content: water vapor (H2O), carbon dioxide (CO2) and Sulfur dioxide (SO2) Outgassing of Volcano Mount St. Helens 1980

Evolution of Atmosphere: 

Evolution of Atmosphere Earth Active plate tectonics “recycles” gases and maintain a moderate atmosphere Venus No plate tectonics to “recycle” gas Once released, remain in the atmosphere, giving a thick atmosphere Runaway greenhouse effect Mars No plate tectonics to “recycle” gas Once removed and locked into rocks, remain in the rocks, giving a thin atmosphere Runaway icehouse effect

Slide33: 

Evolution of Atmosphere: Earth On Earth, H2O and CO2 are recycled Ocean evaporates forming water vapor, which rains down returning to Ocean CO2 dissolves in the water, falling into the ocean CO2 and H2O are incorporated into sedimentary rocks most CO2 is removed from the atmosphere, and locked into the Earth’s rocks. Released through outgassing

Slide34: 

On Venus, the atmosphere experienced a runaway greenhouse effect In the early history, it may also have liquid ocean as Earth Temperature was higher due to stronger radiation from the Sun, because closer to the Sun than the Earth The atmosphere had relatively more water vapor The greenhouse effect of the water vapor raised the temperature, and more liquid water evaporated This further intensified the greenhouse effect, and raised the temperature even higher This runaway process continued until oceans disappeared Almost all of the water vapor was eventually lost by the break-up of molecules due to ultraviolet radiation. Hydrogen escapes into space once it is isolated. Evolution of Atmosphere: Venus

Slide35: 

Without ocean to dissolve in, the outgassed CO2 would accumulate in the Venus’s atmosphere The Earth has roughly as much carbon dioxide as Venus, but it has been dissolved in the Earth’s oceans and chemically bound into its rocks Evolution of Atmosphere: Venus

Slide36: 

On Mars, the atmosphere experienced a runaway icehouse effect Mars originally had a similar thick atmosphere and a liquid water ocean as the early Earth Because Mars is small, it cooled early its history and volcanic activity came to an end Any depletion of carbon dioxide due to rain water was permanent, since no repletion from outgassing. This weakened the greenhouse effect, and caused the temperature to drop A lower temperature caused more water vapor to condense to the surface, carrying carbon dioxide This further reduced the temperature, caused a runaway icehouse effect, opposite to the runaway greenhouse effect occurred on Venus Evolution of Atmosphere: Mars

Slide37: 

The remaining water is frozen underneath the surface Most CO2 is locked in rocks; it is not recycles into the atmosphere. The resulted in a thin Martian atmosphere Evolution of Atmosphere: Mars

Slide38: 

The questions? Is there life on Mars? Was there life on Mars? Was primitive life ever formed on Mars in the ancient Martian oceans? A good answer to these questions will help answer whether there are other lives in the universe. Mars Exploration

Water on Mars: 

Water on Mars No liquid water or rainfall on the planet’s surface today However, liquid water once flowed on Mars, as evident in many surface features Riverbed “Island” carved by flash flood

Slide40: 

Frozen water is contained in polar caps Frozen water is stored in permafrost under the Martian surface There might be enough water to cover the planet to a depth of 500 meters Water on Mars Water Measurement from Mars Odyssey Spacecraft

Exploration : 

Exploration Many spacecraft have been sent to study the Mars, including both orbiting and landing spacecraft In 1970s, Viking 1 and Viking 2 Landers In 1997, Mars Pathfinder Lander called Sojourner In 2004, Mars Exploration Rovers: Spirit and Opportunity Human exploration on Mars is possible in near future

Final Notes on Chap. 11: 

Final Notes on Chap. 11 There are 9 sections in total. Section 1 to 8 are studied. Section 9 (satellites of Mars) is excluded.