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

Home , Acidalia Planitia, Rock Abrasion Tool

Department of Geological Sciences Planetary Geology Group Dr. Michael Wyatt Dr. James Head III 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 Comparison Of Earth and Mars

EARTH MARS Average Surface 15c -63c Temp. Distance from Sun 149,600,000 km 227,940,000 km

Orbital Period 365.2 days 687 days

Rotational Period 24 hours 24.6 hours Number of Moons 1 2

Obliquity (Tilt) 22.5 deg 25.19 deg. * 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. GLOBAL DICOTOMY OF MARS Northern Lowlands of Mars Acidalia Planitia Region

MOLA: NASA/JPL/ASU MARS EXPLORATION

1996 2004

2001

2004 Exploration of Mars

Mars Global Surveyor Mars Odyssey Mars Express Mars Reconnaissance Launched 1996 Launched 2001 Launched 2003 Orbitier Launched 2005

Instruments: Instruments: Instruments: Instruments: •Mars Orbiter •Thermal Emission •High Resolution •Content Camera (CTX) Camera (MOC) Imaging System Stereo Camera •High Resolution Imaging •Mars Orbiter Laser (Themis) (HRSC) Science Experiment Altimeter (MOLA) •Gamma Ray •OMEGA (Mineral (HiRISE) •Thermal Emission Spectrometer (GRS) observations •Compact Reconnaissance Spectrometer (TES) •Martian Radiation Image Spectrometer for Experiment (MARIE) Mars (CRISM) •Mars Color Imager (MARCI) EXPLORATION OF MARS

Mars Pathfinder Sojourner Rover Mars Exploration Rovers: Mars Polar Lander- Phoenix Launched 1996 Spirit and Opportunity Launched 2007 Launched 2003

Instruments: Instruments: Instruments: • Robotic Arm Camera • Alpha Proton X-Ray • Panoramic Camera (RAC) (PANCAM) Spectrometer • Surface Stereo Imager (APXS) • Mini-Thermal Emission (SSI) Spectrometer( Mini-TES) • Imager for Mars • Microscopy, Pathfinder (IMP) • Alpha Particle X-Ray Electrochemistry, and • Atmospheric Spectrometer (APXS) Conductivity analyzer Structure Instrument • MossBauer (MECA) /Meteorology Spectrometer • Thermal and Evolved Package (ASI/MET) • Rock Abrasion Tool Gas Analyzer (TEGA) (RAT) • Mars Descent Imager • Microscopic Imager (MI) (MARDI) • Meteorological Station (MET) GK-12 Summer Research

CURRICULUM RESEARCH PROJECT PROJECT

• Focus on Impact • Northern Craters Lowlands Comparative Planetology Comparing geologic features Comparing mineralogy of of Earth and Mars Earth and Mars

NASA/JPL/ASU Landsat images

Evidence of Jarosite Hematite on Earth

NASA/JPL/ASU 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. Comparison of Craters

Mars Earth’s Moon

• Subsurface water/ice • Ejecta form ray pattern create lobate ejecta • Little modification of • High modification of craters craters NASA/JPL/ASU Research Project:

Driving Question: How does Water/Ice Affect the Surface of Mars?

1. Surface Composition (Minerals)

2. Surface Morphology METHODOLOGY: SATELLITE IMAGERY

MOLA COLOR: Topography MOLA SHADED RELIEF

THEMIS DAY VISABLE TES HIGH CA PYROXENE: Composition

HiRISE HRSC Malin Space Science Systems 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? MOLA Shaded Relief TES Pyroxene 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? Examples of Features to Characterize Surface

Lobe Ejecta Craters Knobs/Mesas

Pitted Mounds Depressions

Wrinkle Ridges Channels

Polygonal Terrain Pedestal Craters 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. 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. Theory Three:

Basaltic material was already present and the surface was altered by water and ice.

Pyroxene band shows the extent of that alteration. • Dissected terrain with mesas in highland/lowland boundary •Wrinkle ridges Mawrth Vallis • Cliffs/scarps • Eroded remains of large craters • Pyroxene evident in area

MOLA Shaded Relief: NASA/JPL/ASU

HiRISE: Mawrth Vallis MOLA Shaded Relief

• Arrows indicate wrinkle ridges • Pedestal remains of large craters • Lobate ejecta patterns around newer craters • Pyroxene evident in area

HiRISE image HiRISE: NASA/JPL/ASU Acidalia Mense

HiRISE: NASA/JPL/ASU

MOLA: NASA/JPL/ASU • Wrinkle ridges not apparent • Many channels present • Depressions • Lobate ejecta craters • Channels • Pitted Mounds • Polygonal terrain • High albedo ejecta around crater lobes • Ghost/eroded craters not evident • Pitted mounds

CTX:NASA/JPL/ASU 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. 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. Mars Phoenix Lander: NASA/JPL/ASU Exploring the Arctic Plains of Mars

Evidence of ice on Mars Acknowledgements

Dr. Michael Wyatt Dr. James Head III Brown Planetary Geology Group

Karen Haberstroh Heather Johnson GK-12 Summer Research Program EXPLORATION OF MARS

Mars Pathfinder Sojourner Rover Mars Exploration Rovers: Mars Polar Lander- Phoenix Launched 1996 Spirit and Opportunity Launched 2007 Launched 2003

Mars Global Surveyor Mars Odyssey Mars Express Mars Reconnaissance Launched 1996 Launched 2001 Launched 2003 Orbitier Launched 2005

USGS: Tanaka, Skinner, and Hare