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Palagonitic Mars from Rock Rinds to Dust: Evidence from Visible, Near-IR, and Thermal Emission Spectra of Poorly Crystalline MaterialsVisible and near-IR (VNIR) spectral data for Martian bright regions are characterized by a general shape consisting of a ferric absorption edge extending from about 400 to 750 nm and relatively constant reflectivity extending from about 750 nm to beyond 2000 nm . Among terrestrial geologic materials, the best spectral analogues are certain palagonic tephras from Mauna Kea Volcano (Hawaii). By definition, palagonite is a yellow or orange isotropic mineraloid formed by hydration and devitrification of basaltic glass. The ferric pigment in palagonite is nanometer-sized ferric oxide particles (np-Ox) dispersed throughout the hydrated basaltic glass matrix. The hydration state of the np-Ox particles is not known, and the best Martian spectral analogues contain allophane-like materials and not crystalline phyllosilicates. We show here that laboratory VNIR and TES spectra of palagonitic alteration rinds developed on basaltic rocks are spectral endmembers that provide a consistent explanation for both VNIR and TES data of Martian dark regions.
Document ID
20030111510
Document Type
Conference Paper
Authors
Morris, R. V. (NASA Johnson Space Center Houston, TX, United States)
Graff, T. G. (Arizona State Univ. Tempe, AZ, United States)
Mertzman, S. A. (Franklin and Marshall Coll. Lancaster, PA, United States)
Lane, M. D. (Planetary Science Inst. Tucson, AZ, United States)
Christensen, P. R. (Arizona State Univ. Tempe, AZ, United States)
Date Acquired
August 21, 2013
Publication Date
January 1, 2003
Publication Information
Publication: Lunar and Planetary Science XXXIV
Subject Category
Lunar and Planetary Science and Exploration
Distribution Limits
Public
Copyright
Public Use Permitted.

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IDRelationTitle20030110578Analytic PrimaryLunar and Planetary Science XXXIV
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