Detection and discrimination of sulfate minerals using reflectance spectroscopy

被引:331
作者
Cloutis, Edward A.
Hawthorne, Frank C.
Mertzman, Stanley A.
Krenn, Katherine
Craig, Michael A.
Marcino, Dionne
Methot, Michelle
Strong, Johnathon
Mustard, John F.
Blaney, Diana L.
Bell, James F., III
Vilas, Faith
机构
[1] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada
[2] Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada
[3] Franklin & Marshall Coll, Dept Geosci, Lancaster, PA 17604 USA
[4] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA
[5] Jet Propuls Lab, Pasadena, CA 91009 USA
[6] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA
[7] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA
基金
加拿大自然科学与工程研究理事会;
关键词
asteroids; composition; Europa; Mars; surface; meteorites; mineralogy; spectroscopy;
D O I
10.1016/j.icarus.2006.04.003
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
A suite of sulfate minerals were characterized spectrally, compositionally, and structurally in order to develop spectral reflectance-compositional-structural relations for this group of minerals. Sulfates exhibit diverse spectral properties, and absorption-band assignments have been developed for the 0.3-26 mu m range. Sulfate absorption features can be related to the presence of transition elements, OH, H2O, and SO4 groups. The number, wavelength position, and intensity of these bands are a function of both composition and structure. Cation substitutions can affect the wavelength positions of all major absorption bands. Hydroxo-bridged Fe3+ results in absorption bands in the 0.43, 0.5, and 0.9 mu m regions, while the presence of Fe2+ results in absorption features in the 0.9-1.2 mu m interval. Fundamental S-O bending and stretching vibration absorption bands occur in the 8-10, 13-18, and 19-24 mu m regions (1000-1250, 550-770, and 420-530 cm(-1)). The most intense combinations and overtones of these fundamentals are found in the 4-5 mu m (2000-2500 cm(-1)) region. Absorption features seen in the 1.7-1.85 mu m interval are attributable to H-O-H/O-H bending and translation/rotation combinations, while bands in the 2.1-2.7 mu m regions can be attributed to H2O- and OH-combinations as well as overtones of S-O bending fundamentals. OH- and H2O-bearing sulfate spectra are fundamentally different from each other at wavelengths below similar to 6 mu m. Changes in H2O/OH content can shift S-O band positions due to change in bond lengths and structural rearrangement. Differences in absorption band wavelength positions enable discrimination of all the sulfate minerals used in this study in a number of wavelength intervals. Of the major absorption band regions, the 4-5 mu m region seems best for identifying and discriminating sulfates in the presence of other major rock-forming minerals. (c) 2006 Elsevier Inc. All rights reserved.
引用
收藏
页码:121 / 157
页数:37
相关论文
共 182 条
[1]  
ADLER HH, 1965, AM MINERAL, V50, P132
[2]  
Alpers C.N., 1994, ACS SYM SER, V550
[3]  
ARLAUCKAS SM, 2004, LUNAR PLANET SCI, V35
[4]   Spectral reflectance and morphologic correlations in eastern Terra Meridiani, Mars [J].
Arvidson, RE ;
Poulet, F ;
Bibring, JP ;
Wolff, M ;
Gendrin, A ;
Morris, RV ;
Freeman, JJ ;
Langevin, Y ;
Mangold, N ;
Bellucci, G .
SCIENCE, 2005, 307 (5715) :1591-1594
[5]  
BAIN RJ, 1990, GEOLOGY, V18, P447, DOI 10.1130/0091-7613(1990)018<0447:DNOFG>2.3.CO
[6]  
2
[7]   MINERALOGIC AND PETROLOGIC IMPLICATIONS OF VIKING GEOCHEMICAL RESULTS FROM MARS - INTERIM-REPORT [J].
BAIRD, AK ;
TOULMIN, P ;
CLARK, BC ;
ROSE, HJ ;
KEIL, K ;
CHRISTIAN, RP ;
GOODING, JL .
SCIENCE, 1976, 194 (4271) :1288-1293
[8]   Experimental hydrothermal alteration of a martian analog basalt: Implications for martian meteorites [J].
Baker, LL ;
Agenbroad, DJ ;
Wood, SA .
METEORITICS & PLANETARY SCIENCE, 2000, 35 (01) :31-38
[9]   Identification of quartzofeldspathic materials on Mars [J].
Bandfield, JL ;
Hamilton, VE ;
Christensen, PR ;
McSween, HY .
JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS, 2004, 109 (E10) :E100091-14
[10]   Acidic volatiles and the Mars soil [J].
Banin, A ;
Han, FX ;
Kan, I ;
Cicelsky, A .
JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS, 1997, 102 (E6) :13341-13356