5sept03 notes

Slide1: 

29:52 Announcements Slight Changes in Syllabus - today (9/5): WATER ON MARS - Monday (9/8): EXPLORATION OF MARS - other topics pushed back Homework #2 due Wednesday, 8 Sept!! - questions from book + one sheet from internet - no PRS Quiz this week – next week Observing Assignment: due NEXT FRIDAY - Clear Sky Patrol Observing - next week Monday-Thursday Free powerpoints at http://www.worldofteaching.com

Slide2: 

Water on Mars Geological Evidence for Water on Mars** - gullies, erosion channels - layers/sedimentary features The Physics of Water on Mars polar ice caps – seasonal variation atmosphere - history Chemical Evidence for Water on Mars Theories for Water on Mars – debates! The Martian Meteorites

Slide3: 

Water on Mars although many images suggest SIGNS of water, NO LIQUID WATER or RAIN has ever been observed! Viking 1 Orbiter MGS One of the most natural human curiosities – related to the ultimate question of LIFE on Mars

Geological Evidence: Outflow Channels: 

Geological Evidence: Outflow Channels Outflow channels suggest that massive floods happened: - water discharge rates ~10,000 times Mississippi River flood - did these floods form into a massive ocean? Ares Valles MGS data

Geological Evidence: Martian Channels: 

Geological Evidence: Martian Channels Martian Gullies: left (Mars) and right (Earth). In the Earth picture, rain water flowing under and seeping along the base of a recently-deposited volcanic ash layer has created the gully. For Mars, water is not actually seen but is inferred from the landforms and their similarity to examples on Earth. Mars Global Surveyor Image (June 2000) Earth (Mt. St. Helens)

Geological Evidence: Sustained Water Flow: 

Geological Evidence: Sustained Water Flow

Slide7: 

MGS

Geological Evidence: Possible Ancient Streambeds and Erosion Channels: 

Geological Evidence: Possible Ancient Streambeds and Erosion Channels

Slide9: 

Summers in the Martian southern hemisphere are shorter than summers in the northern hemisphere. Why? The northern hemisphere is chilled by a larger polar cap There are more volcanoes in the southern hemisphere (3) The southern hemisphere is at much lower elevation on average the Martian equatorial bulge makes the sun shine more directly on the Southern hemisphere (4)This is a consequence of Mars’ elliptical orbit.

Slide10: 

The physics of finding water on Mars When/how does water (H20) exist in its liquid state? LIQUID water exists over a very NARROW range in TEMPERATURE - if T is too high  gas - if T is too low  solid (ice) The TEMPERATURE of water will depend on the ATMOSPHERIC PRESSURE - if Pressure is too low – water will vaporize (evaporate) - if Pressure is too high – water will stay liquid! Mars’ atmospheric pressure is ~1% of Earth’s - LOW pressure - LOW temperature  FROZEN WATER (ice!)

Slide11: 

Mars Global Surveyor TES instrument

Slide12: 

Mars Global Surveyor TES instrument

Slide13: 

Martian Atmosphere Carbon Dioxide (CO2): 95.32% Nitrogen (N2): 2.7% Argon (Ar): 1.6% Oxygen (O2): 0.13% Water (H2O): 0.03% Neon (Ne): 0.00025 % 1/1,000 as much water as our air only enough to cover the surface of the planet with 0.4 inches if melted out of the atmosphere!! Martian atmosphere does not regulate the surface temperature on the planet as Earth’s

Slide14: 

Mars Global Surveyor TES instrument

Slide15: 

History of Mars’ atmosphere: first like Earth’s Atmospheres of terrestrial planets created by out-gassing of volcanoes - ~4 Billion years ago (Mars/Earth = same atmosphere) - volcanic gasses: nitrogen, CO2, water vapor H2O in atmospheres condensed to create oceans on Earth CO2 cycles through our atmosphere: volcanoes/carbonate rocks

Slide16: 

What happened to the atmosphere on Mars? CO2 and H2O may have condensed out and onto the surface – got so cold, that the water froze into permafrost End of volcanic activity, however, would stop the cycle Strong UV light from the Sun will break up chemicals on surface and cause them to evaporate

Storage place for Water: some in N Polar Cap!: 

Storage place for Water: some in N Polar Cap! Caps are frozen carbon dioxide CO2 (‘dry ice’) and some frozen water notes on frozen CO2 - CO2 freezes at T~150 K (~ -200 F) - block of ‘dry ice’ T~ -110 F - sublimes directly ice to gas Southern residual cap is ~300 km across, T ~150 K. Northern cap is ~1,000 km, T~200K (implies mostly water ice b/c CO2 ice would be sublimating)

Slide18: 

Chemical Evidence: Looking for presence of minerals which suggest water Small amounts of water vapor in the atmosphere indicated that much of the planet’s water lost to space – evaporated Recent Mars missions have looked for evidence of carbonates large seafloor beds resulting from consumption of atmospheric CO2 finding little or none – this is problematic, controversial Recent Mars missions have found Hematite – a signature of dried-up lakes on a few places on the planet from TES instrument on MGS

Slide19: 

Recent Chemical Evidence for water on Mars: Detection of Hydrogen (Mars Odyssey - 2003)

Slide20: 

Recent chemical Evidence for water on Mars: Detection of Hydrogen (Mars Odyssey - 2003)

Slide21: 

Theories for Water on Mars: WET, WARM MARS Theories for Water on Mars: COLD, DESERT MARS early atmosphere was dense - could support water in liquid form - could “rain” out the CO2 onto the surface large beds of carbonate form in standing water like on Earth (Oceans) water would be plentiful on Mars, could generate the observed features Never right conditions for water to condense and to create erosions Have to rely on other eroding agents: - wind? - dust? - liquid carbon dioxide?

Slide22: 

Theories for Water on Mars: Current Data & Ideas… Mars probably did have a “warmer, wetter” past, but not extreme - studies show water can exist in ice-covered lakes - as long as temperatures get above freezing for a few days - clues from glacial regions on Earth have helped Geological Evidence: Use Ancient Lakebeds/Glacial Lakes as analogy

Geological Evidence: Layered Sedimentary Features: 

Geological Evidence: Layered Sedimentary Features 141 km (88 miles) Holden Crater

Slide24: 

Also can invoke an active underground system of water - water lower down may be able to be liquid (warmer near Mars’ core) - volcanic soils (megaregolith) are incredibly porous Also can invoke CYCLES of warm, wet climates - volcanic activity generates atmosphere for short periods - water starts flowing again (unfreeze it) - create the observed layers of water erosion features - water freezes into permafrost under Mars surface The final word… keep watching the skies (NASA) Monday: review of current/future Mars Exploration New results in every day! Theories for Water on Mars: Current Data & Ideas…

Slide25: 

What are these “meteorites”? Martian Meteorites Why aren’t they orange – the color of Mars surface? How did they get to Earth? How do we know these meteorites are from Mars? Martian data without going there! Unusual rocks found in Antarctica An impact on Mars (crater size: 10-100 km) ejected part of the Martian surface Chemical composition does not match usual meteorites Only 1.3 billion yrs old (most asteroid-type meteorites MUCH older); Higher content of volatile substances Has to do with how the rocks weathered

Slide26: 

Case Study: Martian Rock ALH84001 Mass = 1.9 kg Igneous Rock Discovered in Antarctica (easier to find) 1984 Formed on Mars 4.5 Billion yr ago Ejected ~16 Million yr ago Landed ~13,000 yr ago What DO they tell us? What DON’T they tell us? Physical processes on Mars Crust/core developed early in Solar System Volcanism until < 1 Billion Years ago Chemical composition Interaction with water Martian atmosphere composition Location of origin Enough about Mars’ water & atmosphere Need to RETURN ROCKS from Mars!!

Slide27: 

Globules of carbonate minerals (the yellow-orange grains) are scattered along cracks in this small chip of ALH 84001. The rims contain iron oxides (including magnetite) and iron sulfides--incompatible minerals that on Earth would suggest microbial action Controversial – microbial presence in meteorites?? Close up views reveal structure similar to Earth microbes!

Slide28: 

Mars has a very thin atmosphere and no magnetosphere. If humans populated the Martian surface, what environmental problems will they be concerned about? Global Warming (2) Solar flare particles and ultraviolet radiation (3) Nitrogen poisoning (4) Lead contamination from volcanoes (5) Magnetic anomalies in the interior causing brain disorders

Slide29: 

Monday: Mars Surface Exploration

Slide30: 

Monday: Mars Surface Exploration