David Baxter. GK-12 Summer Research Program Brown University Oliver Hazard Perry Middle School NASA Explorer School

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1 David Baxter GK-12 Summer Research Program Brown University Oliver Hazard Perry Middle School NASA Explorer School Department of Geological Sciences Planetary Geology Group Dr. Michael Wyatt Dr. James Head III

2 NASA/JPL/ASU Overall Mars Science Strategy: Follow the Water Science Goals of NASA s Long Term Mars Program 1: Determine Whether Life Arose on Mars 2: Characterize the Climate of Mars 3: Characterize the Geology of Mars 4: Prepare for Human Exploration

3 Comparison Of Earth and Mars Average Surface Temp. Distance from Sun Orbital Period Rotational Period Number of Moons Obliquity (Tilt) EARTH 15c 149,600,000 km days 24 hours deg MARS -63c 227,940,000 km 687 days 24.6 hours deg. *

4 OBLIQUITY OF MARS AND EARTH Increased axis tilt causes climatic changes, especially at the poles. These changes in obliquity correspond to warmer climatic patterns. Mars has had a dry and cold climate except for brief periods of high obliquity.

5 GLOBAL DICOTOMY OF MARS

6 MOLA: NASA/JPL/ASU Northern Lowlands of Mars Acidalia Planitia Region

7 MARS EXPLORATION

8 Exploration of Mars Mars Global Surveyor Launched 1996 Mars Odyssey Launched 2001 Mars Express Launched 2003 Mars Reconnaissance Orbitier Launched 2005 Instruments: Mars Orbiter Camera (MOC) Mars Orbiter Laser Altimeter (MOLA) Thermal Emission Spectrometer (TES) Instruments: Thermal Emission Imaging System (Themis) Gamma Ray Spectrometer (GRS) Martian Radiation Experiment (MARIE) Instruments: High Resolution Stereo Camera (HRSC) OMEGA (Mineral observations Instruments: Content Camera (CTX) High Resolution Imaging Science Experiment (HiRISE) Compact Reconnaissance Image Spectrometer for Mars (CRISM) Mars Color Imager (MARCI)

9 EXPLORATION OF MARS Mars Pathfinder Sojourner Rover Launched 1996 Mars Exploration Rovers: Spirit and Opportunity Launched 2003 Mars Polar Lander- Phoenix Launched 2007 Instruments: Alpha Proton X-Ray Spectrometer (APXS) Imager for Mars Pathfinder (IMP) Atmospheric Structure Instrument /Meteorology Package (ASI/MET) Instruments: Panoramic Camera (PANCAM) Mini-Thermal Emission Spectrometer( Mini-TES) Alpha Particle X-Ray Spectrometer (APXS) MossBauer Spectrometer Rock Abrasion Tool (RAT) Microscopic Imager (MI) Instruments: Robotic Arm Camera (RAC) Surface Stereo Imager (SSI) Microscopy, Electrochemistry, and Conductivity analyzer (MECA) Thermal and Evolved Gas Analyzer (TEGA) Mars Descent Imager (MARDI) Meteorological Station (MET)

10 GK-12 Summer Research CURRICULUM PROJECT RESEARCH PROJECT Focus on Impact Craters Northern Lowlands

11 Comparative Planetology Comparing geologic features of Earth and Mars Comparing mineralogy of Earth and Mars Landsat images NASA/JPL/ASU Hematite on Earth Evidence of Jarosite NASA/JPL/ASU

12 Why is the Study of Craters Important? Analyzing the formation, morphology, and modification of craters can: Help determine the relative age of a surface. Determine the geology, as crater formation brings material to the surface. Provide a basis for comparative planetology.

13 Comparison of Craters Mars Earth s Moon Subsurface water/ice create lobate ejecta High modification of craters Ejecta form ray pattern Little modification of craters

14 NASA/JPL/ASU Research Project: Driving Question: How does Water/Ice Affect the Surface of Mars? 1. Surface Composition (Minerals) 2. Surface Morphology

15 METHODOLOGY: SATELLITE IMAGERY MOLA COLOR: Topography MOLA SHADED RELIEF THEMIS DAY VISABLE TES HIGH CA PYROXENE: Composition HiRISE HRSC Malin Space Science Systems

16 ACIDALIA PLANITIA MOLA Shaded Relief: NASA/JPL/ASU Attempt to use geologic surface feature to explain how water and ice have altered the surface in this area. Which geologic process was the most recent?

17 MOLA Shaded Relief TES Pyroxene

18 NASA/JPL/ASU Focus Questions: Explain the occurrence of Basaltic material (pyroxene) in area of the Mawrth Vallis within Acidalia Palnitia. Can surface features of this region explain the geologic history of what happened?

19 Examples of Features to Characterize Surface Lobe Ejecta Craters Knobs/Mesas Pitted Mounds Depressions Wrinkle Ridges Channels Polygonal Terrain Pedestal Craters

20 Theory One: Water transported basaltic material from highlands into the lowlands area through channels during a period of warmer climate. The pyroxene signature shows the extent of these deposits.

21 Theory Two: Basaltic material was already covering entire area and was covered by volcanic Andesite material from the north. The pyroxene signature indicates the extent of that onlapping material.

22 Theory Three: Basaltic material was already present and the surface was altered by water and ice. Pyroxene band shows the extent of that alteration.

23 Mawrth Vallis Dissected terrain with mesas in highland/lowland boundary Wrinkle ridges Cliffs/scarps Eroded remains of large craters Pyroxene evident in area MOLA Shaded Relief: NASA/JPL/ASU HiRISE: Mawrth Vallis

24 MOLA Shaded Relief Arrows indicate wrinkle ridges Pedestal remains of large craters Lobate ejecta patterns around newer craters Pyroxene evident in area HiRISE image

25 Acidalia Mense HiRISE: NASA/JPL/ASU HiRISE: NASA/JPL/ASU MOLA: NASA/JPL/ASU Wrinkle ridges not apparent Many channels present Depressions Lobate ejecta craters Channels Pitted Mounds

26 Polygonal terrain High albedo ejecta around crater lobes Ghost/eroded craters not evident Pitted mounds CTX:NASA/JPL/ASU

27 Summary Mars surface is being continually changed by geologic processes. There is evidence for tectonic activity, volcanism, fluvial (water) processes, etc. The question is which process is the most recent. The climate is largely dry and cold except during brief periods of high obliquity. The geologic features found in areas without pyroxene signature are consistent with ice weathered surfaces. These same features are found in places on Earth such as Antarctica, Greenland, and Iceland.

28 CONCLUSIONS Geologic features suggest the weathering of basalt by water and ice in the Mawrth Vallis area of Acidalia Planitia. Based on evidence, this appears to be the most recent process onlapping older material. The pyroxene band present appears to be the boundary of this weathering. This pyroxene material may have been deposited through channels present during an earlier time of high obliquity.

29 Mars Phoenix Lander: Exploring the Arctic Plains of Mars NASA/JPL/ASU Evidence of ice on Mars

30 Acknowledgements Dr. Michael Wyatt Dr. James Head III Brown Planetary Geology Group Karen Haberstroh Heather Johnson GK-12 Summer Research Program

31 EXPLORATION OF MARS Mars Pathfinder Sojourner Rover Launched 1996 Mars Exploration Rovers: Spirit and Opportunity Launched 2003 Mars Polar Lander- Phoenix Launched 2007 Instruments: Alpha Proton X-Ray Spectrometer (APXS) Imager for Mars Pathfinder (IMP) Atmospheric Structure Instrument /Meteorology Package (ASI/MET) Instruments: Panoramic Camera (PANCAM) Mini-Thermal Emission Spectrometer( Mini-TES) Alpha Particle X-Ray Spectrometer (APXS) MossBauer Spectrometer Rock Abrasion Tool (RAT) Microscopic Imager (MI) Instruments: Robotic Arm Camera (RAC) Surface Stereo Imager (SSI) Microscopy, Electrochemistry, and Conductivity analyzer (MECA) Thermal and Evolved Gas Analyzer (TEGA) Mars Descent Imager (MARDI) Meteorological Station (MET)

32 Exploration of Mars Mars Global Surveyor Launched 1996 Mars Odyssey Launched 2001 Mars Express Launched 2003 Mars Reconnaissance Orbitier Launched 2005 Instruments: Mars Orbiter Camera (MOC) Mars Orbiter Laser Altimeter (MOLA) Thermal Emission Spectrometer (TES) Instruments: Thermal Emission Imaging System (Themis) Gamma Ray Spectrometer (GRS) Martian Radiation Experiment (MARIE) Instruments: High Resolution Stereo Camera (HRSC) OMEGA (Mineral observations Instruments: Content Camera (CTX) High Resolution Imaging Science Experiment (HiRISE) Compact Reconnaissance Image Spectrometer for Mars (CRISM) Mars Color Imager (MARCI)

33 Geologic Map Of Mars USGS: Tanaka, Skinner, and Hare