Surface Exploration of Mars: Past and Future

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Surface eine of Mars: Past Ss ans ian Meteorites ¢ Martian Moons ¢ Martian Surface Exploration The Viking Landers (early 80s) Pathfinder (1997) Current Surface Explorers (three en route!) Future of Martian Exploration (“astrobiology”) ٠ Review of Mars 3 rene) Cc - 0. 0 ‏دنا‎ 0 

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Martian eorites Martian data without going there! What are these Unusual rocks found in Antarctica 0۱ ‏رت‎ ‏ا الف لا‎ Cermes BU ECTeSM Creclici esr <cras OSs LOIN err (cece) Earth? ‏6ع ناك سمتاعة]1 مط غه مهم‎ How do we know these meteorites are fron€harisAl composition does not match usual meteorite Only 1.3 billion yrs old (most asteroid-type meteorites MUCH older); Higher content of volatile substances Why aren’t they orange - the color of 2 ۱ On ‏خخ‎ 

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۱ Crust/core developed early in Solar System Volcanism until < 1 Billion Years ago - Chemical composition Different than normal asteroid (meteorite) Interaction with water Martian atmosphere composition که که ایهم طمنطه: - عحه4ا هم) متوزمه ۵۶ ممت‌گلا الما توفطا 10۸۲۳۲ نعط۲۱۷ 0 - Need to actually RETURN ROCKS from Mars! Case Study: Martian Rock و" ‎too eat i)‏ ی bcted ~16 Million yr ago ded ~13,000 yr ago 3 .0 0۰ - میرظ) ما عون 

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Controversial - microbial presence in meteorites?? biology: exciting field of research - study of origin of life in the solar system,u - LIFE IS UBIQUITOUS in the universe - we just haven't found it Pee RCP RS DUONm nae citi e UCR u Cem cone 

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1۷۲۸۲ ‏صهنا‎ ‎¥ Two Nelo) estes _ Phobos ¥ Small (~20km) irregularly shaped ¥ Orbit Mars in 8hr, 30hr Sas anol ya ‏ل نكا‎ asteroids fori ertetroree roel eemookhobos (20 km.& Qbo-0.0. to. Eros 3 km) (33 km x 13 km) 

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Risks of Solar System Missions ane CONS for Space Missions PROS for Space Missions تمه که خصمصوننوه اعماق امد جع + ۱ that are possible ۲ ۱ ‏ور و‎ ccm they + Much much more costly! (although Y Access to wavelengths that ‏صقطا لعمصممم عه؟ بو1أدمء عتمم‎ are unavailable on the ۱۳۰ ground متعمده تزللمناهنا فا فهستاه‌گنا ‎٩‏ Y Atmospheric effects gone - get clearer views than on ‏اا‎ غلتعةقتة ممه طعناحم دمفهجومل] + کر الس ا 0 ‎Development of‏ ¥ ‎Lee eS oN 0‏ مها فعاه اهوم 0 

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Viking Landers 1 and 2 5 .م56 صذ لعطعصتته1 2 وصغلت! ,1975 06 ۱ * Vikings arrived at Mars in June, August of 1976 Rove yt aes enter eem Ovens ised lo tR ester tte No ot Ace WR To) ee Dag OUCE LU aaa ae On ual ۳ ‎terete ۱‏ )@ ل ل ل ل ل اا 

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Viking Lander Images of Mars’ ۶ 5 + landing site chosen from Orbiter images - two different regions in Northern Lowlands * revealed that the surface of Mars was littered with jagged rocks and fine dust everywhere * rocks were probably result of crater-forming impact (“ejecta”) ©reeksresemble lava-rock$nEarti-Tave flows broken up by impatts 

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Viking Landers: Search for Life on Mars * Science Instruments: - chem lab to explore reactions of Mars rock with water (none detected) - ‏للا حصح 0000و‎ found that the soil was IRON-rich * confined to study only one part of Martian surface - its landing site * inspired NASA to propose for missions with MOVING surface 0 0 - مرهج ۵9و سوه 6 

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Mars has a very thin atmosphere and no magnetosphere. If humans populated the Martian surface, what environmental pam MIAN ‏ات ل‎ (1) Global Warming (2) Solar flare particles and ultraviolet radiation (3) Nitrogen poisoning (4) Lead contamination from volcanoes (5) Magnetic anomalies in the interior 0 ‏ل‎ eA. ea ao 

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ars Pathfinder Mission - landed on Mars 4 July 19¢ ae a landed 500 miles from Vikings - flood plain area olcanic rocks with silicon 00 

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۱۰۱۱ ‏و‎ eee ROVERS Opportunity & Spirit (or MER A and ¢ Launched in June and July of 2003 * arrival at Mars - January 2004 * Each Rover weighs 180 kg, is | ~5 ft high * surface exploration: travels 100m per ‏بصنا .0 .0 - ممحرقا سادق د‎ 06 

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EDL Process % —— - Entry Tum & HRS Freon Veniing:E- 15:00 1. Cruiso Stago Separaton:E-025:00 * ‏ومع‎ £08, 125km 5.7kms, y=-11 Seq ‏وت‎ - Prakhoaing/Decoleraton: <59 Wiend, <8 9 + Parachute Deployment:E+ 295 6 11.8 km 430 m/s 5 + Heatshield Separaton:E+ 915s ‏ع‎ + Lander Separation: £4 9258 + Bridle Deployed:E+ 9953 + Radar Ground Acquisition: L- 18» ۶ + Airbag inflation: 955m Landing 1 ۰ + RocketFiring: L- 7s, -150m, 00 ms + Bridle Gut-L-3s, 20m sLanding:-E+ 420.8 اس ‎Rollto a Stop: Base Petal Down, Landing + 2 min‏ + ‎Latch Firing:Landing + 20 min‏ انا ۱۳ 3 ‎74min‏ + 90 وک نی > ‎“alo aga Opened‏ eae ace XY Bete el ‏صو ند‎ EDL Done @ 1450LST Earth Set @ 1520LST Mars Rover Entry Sequence 

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00 Rae ‏ا ا ا ا‎ Metts cts 

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Choosing a site to land on Mars not just land anywhere - need to consider the safety of the - previous missions have landed in the northern lowlands corer ‏یات‎ Gok Gystew - 0. C. bag, a 

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Mars Landing Considerations اموت ل ‎altitude (impossible climbs, falls)‏ - ‎slopes (use too much energy)‏ - ‎rockiness (protect airbags)‏ - * solar panel heating - keep rover operab! ‎y‏ ك2 ‎solar panels clear‏ - ‎RAT tool works more in thick dust‏ - ‎6 ‏۵9و سوه‎ 0 ae 

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Science Objectives of the MER mission Characterize a variety of rocks and soils that hold clues to past water ¢ .e. try to identify carbonates (indicate water-volcano cycles) ’ Distribution and composition of minerals, rocks, and soils near sites * Determine geologic processes have shaped the local terrain * Perform "ground truth" calibration and validation - of surface observations made ‏کا معط تمانطاده عبع توط‎ مرن سوه رت 

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تسمعصدط ‎IR Spectrometer‏ X-ray Spectrometer 

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Landing Sites on Mars: 1. Gusev Crater - morphological - 15 degrees South of Mars’ equator - large crater feature ‏نتب این‎ 5 oes leading into ne 217 هه 2 مسا 1ك 

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Landing Sites on Mars: 2. Meridiani Planum - mineralogical - 2 degrees South of Mars’ equator - other side of planet from Landing Site 1 - place where hematite has been found (rust-like mineral) - Pan mrenc! dried lake bed 1 60 دنارق 

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Mars Express - European Effort 

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MARS EXPRESS: Radar Experiment Be ee eraced eters t ntl ‏ی‎ ‎of water is very different from rock * Echoes can differentiate between rock and ice or water ۷۵۳ ‏اعیی‎ * Radar transmitter operates at 1-2 MHz and penetrates ground to several km depth * Probably cannot distinguish between CO, and H,0. 3 rene) 

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MARSIS Surface echo 2 Water reservoir Subsurface echo 

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Mars Surface Exploration - the Futur 

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Mars Surface Exploration - the Future! 

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‘uture Mars Exploration: “Scout Missions” + lightweight/efficient ballons * fleet of small aircraft to explore Mars * develop new technology * also SAMPLE RETURNS 

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Surface Exploration of Mars: Past & Future • Martian Meteorites • Martian Moons • Martian Surface Exploration The Viking Landers (early 80s) Pathfinder (1997) Current Surface Explorers (three en route!) Future of Martian Exploration (“astrobiology”) • Review of Mars 8 Sept 2003 Solar System - C. C. Lang 1 Martian Meteorites Martian data without going there! What are these Unusual rocks found in Antarctica “meteorites”? How did they get to An impact on Mars (crater size: 10-100 km) ejected Earth? part of the Martian surface How do we know these meteorites are fromChemical Mars? composition does not match usual meteorite Only 1.3 billion yrs old (most asteroid-type meteorites MUCH older); Higher content of volatile substances Why aren’t they orange – the color of Mars surface? Has to do with how the rocks weathere 8 Sept 2003 Solar System - C. C. Lang 2 What DO they tell us? processes on Mars -Physical Crust/core developed early in Solar System Volcanism until < 1 Billion Years ago - Chemical composition Different than normal asteroid (meteorite) Interaction with water Martian atmosphere composition What DON’T they tell- us? Location of origin (on Mars – which part of surfa - Enough about Mars’ water & atmosphere - Need to actually RETURN ROCKS from Mars!! 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 8 Sept 2003 Solar System - C. C. Lang 3 Controversial – microbial presence in meteorites?? Close up views reveal structure similar to Earth microbes? 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 obiology: exciting field of research – study of origin of life in the solar system,u - LIFE IS UBIQUITOUS in the universe – we just haven’t found it - LIFE IS A SPECIALSolar quirk of -nature 8 Sept 2003 System C. C. Langand timing – very very rare! 4 Martian  Two Moons moons: Deimos, Phobos Small (~20km) irregularly shaped  Orbit Mars in 8hr, 30hr  Probably captured asteroids Deimos Phobos (20 kmSolar x System 27 - C. C. Lang km) 8 Sept 2003 Comparison: Asteroid Eros 5 (33 km x 13 km) Risks of Solar System Missions PROS for Space Missions CONS for Space Missions + Can not fix/test equipment as easily  Closest views of the planets that are possible  Access to wavelengths that are unavailable on the ground  Atmospheric effects gone – get clearer views than on Earth + Large risk with rocket launch + Much much more costly! (although more costly for manned than unmanned) + Lifetime is usually shorter + Upgrades much more difficult + Risks from UV radiation, cosmic rays  Development of sophisticated tech. and 8 Sept 2003 Solar System - C. C. Lang research 6 Viking Landers 1 and 2 • Viking 1 launched in August of 1975, Viking 2 launched in Sept. 1975 • Vikings arrived at Mars in June, August of 1976 • Orbiter + Lander – Orbiters alone weighed close to a ½ ton each – very expensive launch/rocket equipment !! 8 Sept 2003 Solar System - C. C. Lang 7 - these days NASA’s mantra: “Faster Better Cheaper” Viking Lander Images of Mars’ Surface • landing site chosen from Orbiter images – two different regions in Northern Lowlands • revealed that the surface of Mars was littered with jagged rocks and fine dust everywhere • rocks were probably result of crater-forming impact (“ejecta”) Sept 2003 Solar - C.– C. Lang flows broken up by impacts 8 •8rocks resemble lava-rocks onSystem Earth lava Viking Landers: Search for Life on Mars • Science Instruments: - chem lab to explore reactions of Mars rock with water (none detected) - scoop arm with magnet – found that the soil was IRON-rich • confined to study only one part of Martian surface – its landing site 8 Sept 2003 • inspired NASA to propose for missions with MOVING Solar System - C. C. Lang 9 surface Mars has a very thin atmosphere and no magnetosphere. If humans populated the Martian surface, what environmental problems will they be concerned about? (1) 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 Solar disorders 8 Sept 2003 System - C. C. Lang 10 Mars Pathfinder Mission – landed on Mars 4 July 199 Demonstration mission for “Faster Better Cheaper” NASA mantra • used lightweight airbags to land • small, efficient robotic vehicle • 10x as many images as previous missions (compute • landed 500 miles from Vikings – flood plain area (volcanic rocks with silicon) 8 Sept 2003 Solar System - C. C. Lang 11 Panoramic View from Mars’ Pathfinder’s Sojourner Rove 8 Sept 2003 Solar System - C. C. Lang 12 ATHENA: MARS EXPLORATION ROVERS Opportunity & Spirit (or MER A and MER B) • Launched in June and July of 2003 Rover Rover • arrival at Mars – January 2004 • Each Rover weighs 180 kg, is ~5 ft high • surface exploration: travels 100m per day8 Sept 2003 Solar System - C. C. Lang 13 ATHENA: MARS EXPLORATION ROVER Mars Mars Rover Rover 8 Sept 2003 Entry Entry Sequence Solar System - C. C. Lang 14 cartoon of the “airbag” landing of the Mars Exploration Rovers on surface 8 Sept 2003 Solar System - C. C. Lang 15 Choosing a site to land on Mars not just land anywhere – need to consider the safety of the - previous missions have landed in the northern lowlands 8 Sept 2003 Solar System - C. C. Lang 16 Mars Landing Considerations • terrain - altitude (impossible climbs, falls) - slopes (use too much energy) - rockiness (protect airbags) • solar panel heating – keep rover operabl • dust - solar panels clear - RAT tool works more in thick dust 8 Sept 2003 Solar System - C. C. Lang 17 Science Objectives of the MER mission Characterize a variety of rocks and soils that hold clues to past water a i.e. try to identify carbonates (indicate water-volcano cycles) • Distribution and composition of minerals, rocks, and soils near sites • Determine geologic processes have shaped the local terrain • Perform "ground truth" – calibration and validation – of surface observations made by Mars orbiter instruments. 8 Sept 2003 Solar System - C. C. Lang 18 Mars Exploration Rover: Science Instruments Pancam- Stereo camera IR Spectrometer rock composition X-ray Spectrometer - soil and rock chemistry RAT - rock abrasion tool Microscopic imager (search for fossils?) 8 Sept 2003 Solar System - C. C. Lang 19 Landing Sites on Mars: 1. Gusev Crater morphological - 15 degrees South of Mars’ equator - large crater feature with several ‘channels’ leading into it - water may have pooled in crater during first 2 billion years “channel” 8 Sept 2003 Solar System - C. C. Lang 20 Landing Sites on Mars: 2. Meridiani Planum mineralogical - 2 degrees South of Mars’ equator - other side of planet from Landing Site 1 - place where hematite has been found (rust-like mineral) – indicates that it is a former dried lake bed 8 Sept 2003 Solar System - C. C. Lang 21 Mars Express – European Effort 8 Sept 2003 Solar System - C. C. Lang 22 MARS EXPRESS • Launched June 2003 • Radar instrument (MARSIS) built at University of Iowa (Prof. D. Gurnett, P.I.) • other instruments, including a small rover called “Beagle 2” 8 Sept 2003 Solar System - C. C. Lang 23 MARS EXPRESS: Radar Experiment • Radar reflection signal of water is very different from rock • Echoes can differentiate between rock and ice or water • Radar transmitter operates at 1-2 MHz and penetrates ground to several km depth • Probably cannot distinguish between CO2 and H20. 8 Sept 2003 Solar System - C. C. Lang 24 8 Sept 2003 Solar System - C. C. Lang 25 Mars Surface Exploration – the Future! 8 Sept 2003 Solar System - C. C. Lang 26 Mars Surface Exploration – the Future! 8 Sept 2003 Solar System - C. C. Lang 27 Future Mars Exploration: “Scout Missions” • • • • 8 Sept 2003 lightweight/efficient ballons fleet of small aircraft to explore Mars develop new technology also SAMPLE RETURNS Solar System - C. C. Lang 28 Martian Outpost: 2030 8 Sept 2003 Solar System - C. C. Lang 29 8 Sept 2003 Solar System - C. C. Lang 30 This powerpoint was kindly donated to www.worldofteaching.com http://www.worldofteaching.com is home to over a thousand powerpoints submitted by teachers. This is a completely free site and requires no registration. Please visit and I hope it will help in your teaching. 8 Sept 2003 Solar System - C. C. Lang 31