Global mapping of Martian hematite mineral deposits: Remnants of water‐driven processes on early Mars

By Philip R. Christensen, R. Morris, M. Lane, J. Bandfield, Michael C. Malin. 2001

345 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Paleontology, Renewable Energy, Sustainability and the Environment

View Paper: https://www.semanticscholar.org/paper/24e379db1dd198c22daa0b7a21efede03a084216

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Michael D. Smith
2. Philip R. Christensen
3. V. Hamilton
4. J. Bandfield
5. H. McSween
6. James W. Head III
7. Michael J. Wolff
8. W. Koeppen

In Paleontology

1. V. Hamilton
2. David C. Catling
3. Philip R. Christensen
4. H. McSween
5. Andrew H. Knoll
6. James W. Head III
7. S. McLennan
8. Jeffrey Moore

In Renewable Energy, Sustainability and the Environment

1. V. Hamilton
2. David C. Catling
3. Philip R. Christensen
4. Andrew H. Knoll
5. Ralph E. Milliken
6. J. F. Mustard

Citations in the corpus

• Sequence and timing of conditions on early Mars (2011, background): “…been revolutionized by observations in the last decade across the electromagnetic spectrum, first in the thermal infrared by TES and THEMIS (e.g., Christensen et al., 2001; Wyatt and McSween, 2002; Osterloo et al., 2008), and more recently, in the visible to near-infrared, by OMEGA (Gendrin et…”
• Identification of quartzofeldspathic materials on Mars (2004, background): “Exposures of grey crystalline hematite are located in Sinus Meridiani, Aram Chaos, and Ophir and Candor Chasmas [Christensen et al., 2000, 2001a].”
• Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars (2003, methodology): “A detailed description of the instrument can be found in Christensen et al. (1992, 2001a).”
• The nature of coarse-grained crystalline hematite and its implications for the early environment of Mars (2003, methodology): “In certain solutions, the photo-oxidation proc starts with the formation of an iron complex and iron is o dized by the photo-stimulated release of hydrogen gas: Fe2+ + H2O= [Fe(OH)]+ + H+, 2[Fe(OH)]+ + 2H+ + hν → 2Fe(OH)2+ + H2, Fe(OH)2+ + 2H2O↔ Fe(OH)3 + 2H+.”
• Sedimentary silica on Mars (2003, background): “These deposits generally are thought to result from surficial processes, including deposition from low-temperature aqueous solutions, diagenetic processes, or hydrothermal processes (Christensen et al., 2000, 2001; Hynek et al., 2002).”
• Mineralogy and evolution of the surface of Mars: A review (2007, background): “The interpretation of these haematite deposits makes rise multiple hypothesises: precipitations in sedimentary environments from iron-rich waters (Baldridge and Calvin, 2004; Christensen et al., 2001) or organic solvents (Tang et al.”
• Compact Reconnaissance Imaging Spectrometer for Mars investigation and data set from the Mars Reconnaissance Orbiter's primary science phase (2009, methodology): “Global mapping by TES revealed only limited evidence for altered phases, namely coarse-grained hematite associated with Hesperian-aged layered deposits in Meridiani Planum and Valles Marineris [ Christensen et al., 2001a ], and furthermore revealed extensive outcrops of olivine that would easily hav”
• Mars Global Surveyor Thermal Emission Spectrometer experiment: Investigation description and surface science results (2001, background): “Candor region of Valles Marineris [Christensen et al., 2001].”
• The Thermal Emission Imaging System (THEMIS) for the Mars 2001 Odyssey Mission (2004, background): “The spectra of the key minerals shown in Figures 4 and 5 at TES spectral resolution are reproduced in Figure 7 at THEMIS resolution by convolving the laboratory spectra with the THEMIS filter response functions (see Section 4.2).”
• Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “However, those regions and the spatial outlines of the distributions of spectra identified correspond directly to regions previously identified as hematite-rich [ Christensen et al., 2001b ].”
• Overview of the Opportunity Mars Exploration Rover mission to Meridiani Planum: Eagle crater to Purgatory ripple (2006, background): “…of Meridiani geology, not least because a surface veneer of these spherules, eroded from outcrop rocks, carries the remotely sensed spectral signature of hematite that motivated landing on the Meridiani plains [Christensen et al., 2000, 2001; Golombek et al., 2003; Squyres et al., 2004a].”