%0 Journal Article %1 BLANEY1995a %A BLANEY, D. L. %A MCCORD, T. B. %D 1995 %J Journal of Geophysical Research-Planets %K CARBONATES; DUST MARS; ORIGIN; REFLECTANCE; SPECTRA; SURFACE; %N E7 %P 14433--14441 %T INDICATIONS OF SULFATE MINERALS IN THE MARTIAN SOIL FROM EARTHBASED SPECTROSCOPY %V 100 %X Telescopic measurements of Mars between 4.40 and 5.13 mu m at a spectral resolution (lambda/Delta lambda) of 300 were made on August 19, 1988, UT at the NASA infrared Telescope Facility on Mauna Kea, Hawaii. This wavelength region contains radiation from both solar reflection and thermal emission. Additionally, the Martian atmosphere has numerous atmospheric gas absorption features, dominated by the 4.2-mu m CO2 fundamental band. The Mars spectrum rise out of the 4.2 to 4.4-mu m CO2 band on the long-wavelength side cannot be matched solely by atmospheric gas constituents. An absorption must be added at roughly 4.5 mu m in order to decrease the reflectance rise and produce the 4.5-mu m inflection which is present in the data. The location of this feature at the position of the 2 nu 3 overtone of the SO42- anion indicates that the surface absorption is probably caused by sulfates on the Martian surface and/or in atmospheric dust, This is consistent with the known presence of sulfates on the Martian surface from the Viking results. An exact spectral match to a terrestrial sulfur mineral has not been made, but we suggest that the mineral on Mars has very weak band structure, probably due to an ion environment in the mineral with a high degree of electric field symmetry. Significant variation exists at 4.5 mu m among the observed spectra for different locations on Mars. In order of strength, from strongest absorption to weakest, are Eastern Solis Planum, Argyre Basin, Eastern Tharsis, and Valles Marineris for the four regions measured at similar Mars atmospheric conditions.

@article{BLANEY1995a, abstract = {Telescopic measurements of Mars between 4.40 and 5.13 mu m at a spectral resolution (lambda/Delta lambda) of 300 were made on August 19, 1988, UT at the NASA infrared Telescope Facility on Mauna Kea, Hawaii. This wavelength region contains radiation from both solar reflection and thermal emission. Additionally, the Martian atmosphere has numerous atmospheric gas absorption features, dominated by the 4.2-mu m CO2 fundamental band. The Mars spectrum rise out of the 4.2 to 4.4-mu m CO2 band on the long-wavelength side cannot be matched solely by atmospheric gas constituents. An absorption must be added at roughly 4.5 mu m in order to decrease the reflectance rise and produce the 4.5-mu m inflection which is present in the data. The location of this feature at the position of the 2 nu 3 overtone of the SO42- anion indicates that the surface absorption is probably caused by sulfates on the Martian surface and/or in atmospheric dust, This is consistent with the known presence of sulfates on the Martian surface from the Viking results. An exact spectral match to a terrestrial sulfur mineral has not been made, but we suggest that the mineral on Mars has very weak band structure, probably due to an ion environment in the mineral with a high degree of electric field symmetry. Significant variation exists at 4.5 mu m among the observed spectra for different locations on Mars. In order of strength, from strongest absorption to weakest, are Eastern Solis Planum, Argyre Basin, Eastern Tharsis, and Valles Marineris for the four regions measured at similar Mars atmospheric conditions.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {BLANEY, D. L. and MCCORD, T. B.}, biburl = {https://www.bibsonomy.org/bibtex/2fbeda154b36d0c75f595679909cad808/svance}, citedreferences = {ALLEN CW, 1976, ASTROPHYSICAL QUANTI ; BEER R, 1971, Icarus, V15, P1 ; BLANEY DL, 1989, J GEOPHYS RES-SOLID, V94, P10159 ; CALVIN WM, 1994, J GEOPHYS RES-PLANET, V99, P14659 ; CALVIN WM, 1994, J GEOPHYS RES-PLANET, V99, P21143 ; CAMPBELL IB, 1987, ANTARCTICA SOILS WEA, V16 ; CLARK BC, 1982, J GEOPHYS RES, V87, P10059 ; CLARK RN, 1980, PUBL ASTRON SOC PAC, V92, P221 ; ENCRENAZ T, 1990, J GEOPHYS RES-SOLID, V95, P14589 ; EVANS DL, 1980, 11TH P LUN PLAN SCI, P757 ; GOODING JL, 1988, GEOCHIM COSMOCHIM AC, V52, P909 ; Greeley R, 1981, REV GEOPHYS SPACE PH, V19, P13 ; HANEL RA, 1973, NASA TM70504 TECH ME ; HERR KC, 1969, Science, V166, P496 ; HOUCK JR, 1973, Icarus, V18, P470 ; MCCORD TB, 1982, J GEOPHYS RES, V87, P3021 ; MOROZ VI, 1964, SOV ASTRON, V8, P273 ; MUSTARD JF, 1993, J GEOPHYS RES, V98, P3387 ; NASH DB, 1986, APPL OPTICS, V25, P2427 ; POLLACK JB, 1990, J GEOPHYS RES-SOLID, V95, P14595 ; ROUSH TL, 1986, LUNAR PLANET SCI, V13, P661 ; SETTLE M, 1979, J GEOPHYS RES, V84, P8343 ; SINGER RB, 1982, J GEOPHYS RES, V87, P10159 ; SINTON WM, 1957, APJ, V126, P231 ; SINTON WM, 1967, Icarus, V6, P222 ; TOKUNAGA AT, 1987, INFRARED ASTRONOMY A, P367 ; TOULMIN P, 1977, J GEOPHYS RES, V82, P4625 ; WARREN PH, 1987, Icarus, V70, P153}, interhash = {cd2f91cb78fc13450296fd31d720802e}, intrahash = {fbeda154b36d0c75f595679909cad808}, journal = {Journal of Geophysical Research-Planets}, keywords = {CARBONATES; DUST MARS; ORIGIN; REFLECTANCE; SPECTRA; SURFACE;}, number = {E7}, owner = {svance}, pages = {14433--14441}, timestamp = {2009-11-03T20:21:39.000+0100}, title = {INDICATIONS OF SULFATE MINERALS IN THE MARTIAN SOIL FROM EARTHBASED SPECTROSCOPY}, volume = 100, year = 1995 }