Remote Compositional Analysis Techniques for Understanding Spectroscopy, Mineralogy, and Geochemistry of Planetary Surfaces
Book contents
- Remote Compositional Analysis
- Cambridge Planetary Science
- Remote Compositional Analysis
- Copyright page
- Contents
- Contributors
- Foreword
- Preface
- Acknowledgments
- Part I Theory of Remote Compositional Analysis Techniques and Laboratory Measurements
- Part II Terrestrial Field and Airborne Applications
- Part III Analysis Methods
- Part IV Applications to Planetary Surfaces
- 17 Spectral Analyses of Mercury
- 18 Compositional Analysis of the Moon in the Visible and Near-Infrared Regions
- 19 Spectral Analyses of Asteroids
- 20 Visible and Near-Infrared Spectral Analyses of Asteroids and Comets from Dawn and Rosetta
- 21 Spectral Analyses of Saturn’s Moons Using the Cassini Visual Infrared Mapping Spectrometer
- 22 Spectroscopy of Pluto and Its Satellites
- 23 Visible to Short-Wave Infrared Spectral Analyses of Mars from Orbit Using CRISM and OMEGA
- 24 Thermal Infrared Spectral Analyses of Mars from Orbit Using the Thermal Emission Spectrometer and Thermal Emission Imaging System
- 25 Thermal Infrared Remote Sensing of Mars from Rovers Using the Miniature Thermal Emission Spectrometer
- 26 Compositional and Mineralogic Analyses of Mars Using Multispectral Imaging on the Mars Exploration Rover, Phoenix, and Mars Science Laboratory Missions
- 27 Mössbauer Spectroscopy at Gusev Crater and Meridiani Planum
- 28 Elemental Analyses of Mars from Rovers Using the Alpha-Particle X-Ray Spectrometer
- 29 Elemental Analyses of Mars from Rovers with Laser-Induced Breakdown Spectroscopy by ChemCam and SuperCam
- 30 Neutron, Gamma-Ray, and X-Ray Spectroscopy of Planetary Bodies
- 31 Radar Remote Sensing of Planetary Bodies
- Index
- References
23 - Visible to Short-Wave Infrared Spectral Analyses of Mars from Orbit Using CRISM and OMEGA
from Part IV - Applications to Planetary Surfaces
Published online by Cambridge University Press: 15 November 2019
Book contents
- Remote Compositional Analysis
- Cambridge Planetary Science
- Remote Compositional Analysis
- Copyright page
- Contents
- Contributors
- Foreword
- Preface
- Acknowledgments
- Part I Theory of Remote Compositional Analysis Techniques and Laboratory Measurements
- Part II Terrestrial Field and Airborne Applications
- Part III Analysis Methods
- Part IV Applications to Planetary Surfaces
- 17 Spectral Analyses of Mercury
- 18 Compositional Analysis of the Moon in the Visible and Near-Infrared Regions
- 19 Spectral Analyses of Asteroids
- 20 Visible and Near-Infrared Spectral Analyses of Asteroids and Comets from Dawn and Rosetta
- 21 Spectral Analyses of Saturn’s Moons Using the Cassini Visual Infrared Mapping Spectrometer
- 22 Spectroscopy of Pluto and Its Satellites
- 23 Visible to Short-Wave Infrared Spectral Analyses of Mars from Orbit Using CRISM and OMEGA
- 24 Thermal Infrared Spectral Analyses of Mars from Orbit Using the Thermal Emission Spectrometer and Thermal Emission Imaging System
- 25 Thermal Infrared Remote Sensing of Mars from Rovers Using the Miniature Thermal Emission Spectrometer
- 26 Compositional and Mineralogic Analyses of Mars Using Multispectral Imaging on the Mars Exploration Rover, Phoenix, and Mars Science Laboratory Missions
- 27 Mössbauer Spectroscopy at Gusev Crater and Meridiani Planum
- 28 Elemental Analyses of Mars from Rovers Using the Alpha-Particle X-Ray Spectrometer
- 29 Elemental Analyses of Mars from Rovers with Laser-Induced Breakdown Spectroscopy by ChemCam and SuperCam
- 30 Neutron, Gamma-Ray, and X-Ray Spectroscopy of Planetary Bodies
- 31 Radar Remote Sensing of Planetary Bodies
- Index
- References
Summary
Visible to short-wave infrared (VSWIR, 0.4–5.0 µm) reflectance spectroscopy is a powerful tool to identify and map mineral groups on the martian surface. The Mars Express/OMEGA and Mars Reconnaissance Orbiter/CRISM instruments have characterized more than 30 mineral groups, revolutionizing previous understanding of martian crustal composition and the role of water in altering it. Analyses of these spectral images revealed the primary structure of the crust to be dominated by basalt, over a deep layer of segregated pyroxene- and olivine-rich plutons, with sparse feldspar-rich, differentiated intrusions. Martian volatile-bearing environments have evolved through four phases: the pre-Noachian to early Noachian period when alteration by liquid water occurred near the surface and deep in the subsurface, in chemically neutral to alkaline environments that formed hydrous silicates and carbonates; the middle to late Noachian period when liquid water was widely present at the surface forming valley networks, lacustrine deposits, and clay-rich pedogenic horizons; the early Hesperian to early Amazonian period during which water became increasingly acidic and saline, forming deposits rich in sulfate salts, chlorides, and hydrated silica; and the Amazonian period when surface water has existed predominantly as ice, with only localized reaction with regolith and briny flow on the surface.
Keywords
- Type
- Chapter
- Information
- Remote Compositional AnalysisTechniques for Understanding Spectroscopy, Mineralogy, and Geochemistry of Planetary Surfaces, pp. 453 - 483Publisher: Cambridge University PressPrint publication year: 2019
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