Effects of Palagonitic and Basaltic Dust Coatings on Visible, Near-IR, Thermal Emission and Moessbauer Spectra of Rocks and Minerals: Implications for Mineralogical Remote Sensing of Mars

Details Effects of Palagonitic and Basaltic Dust Coatings on Visible, Near-IR, Thermal Emission and Moessbauer Spectra of Rocks and Minerals: Implications for Mineralogical Remote Sensing of Mars Effects of Palagonitic and Basaltic Dust Coatings on Visible, Near-IR, Thermal Emission and Moessbauer Spectra of Rocks and Minerals: Implications for Mineralogical Remote Sensing of Mars

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p72a0486g&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #P72A-0486

Mathematics

Logic

5464 Remote Sensing, 5470 Surface Materials And Properties, 5494 Instruments And Techniques

Scientific paper

Dust coatings on the surface of Mars complicate and, if sufficiently thick, mask the detection of the mineralogical signatures of the underling material from remote sensing instrumentation aboard orbiters, landers and rovers. An air-fall method for depositing fine-grained material (<50 microns) was developed to uniformly coat rock (basalt, andesite, kaolinite and quartz claystone, schistose hematite) and mineral (olivine, pyroxmangite, siderite) substrates to thicknesses up to ~2000 microns. Dust analogs used to date include, palagonite from the summit region of Mauna Kea Volcano (Hawaii) and crushed basaltic material from Mulcahy Lake (Canada). The method allows for the determination of spectral effects resulting from various thicknesses of dust accumulation with numerous experiment techniques (visible, near-IR, thermal emission and backscatter Moessbauer spectroscopy). Results demonstrate that infinite optical thickness in the visible wavelengths (350-700 nanometers) is on the order of 10-35 and 10-55 microns for palagonitic and basaltic dust coatings, respectively. Band features for all the substrates were complete diminished in the near-IR (700-2100 nanometers) with coatings of ~300 microns for both dust analogs. In the thermal emission spectra (2000-200 wavenumbers) the emissivity spectrum of the substrate was obscured with dust thicknesses of 150-250 microns. Palagonitic dust coatings ~2000 microns thick (~25 mg/cm2) were not sufficient to mask the substrate material from the 14.4 kev gamma-rays used in the Moessbauer experiments.

Affiliated with

Also associated with

No associations

Rating

Effects of Palagonitic and Basaltic Dust Coatings on Visible, Near-IR, Thermal Emission and Moessbauer Spectra of Rocks and Minerals: Implications for Mineralogical Remote Sensing of Mars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Effects of Palagonitic and Basaltic Dust Coatings on Visible, Near-IR, Thermal Emission and Moessbauer Spectra of Rocks and Minerals: Implications for Mineralogical Remote Sensing of Mars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Effects of Palagonitic and Basaltic Dust Coatings on Visible, Near-IR, Thermal Emission and Moessbauer Spectra of Rocks and Minerals: Implications for Mineralogical Remote Sensing of Mars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1892373