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Spectral properties of simulated impact glasses produced from Martian soil analogue JSC Mars-1

Moroz, L.V. und Basilevsky , A.T. und Hiroi, T. und Rout, S.S. und van der Bogert, C.H. und Yakovlev, O.I. und Fisenko, A.V. und Semjonova, L.F. und Rusakov, V.S. und Khramov, D.A. und Zinovieva, N.G. und Arnold, G. und Pieters, C.M. (2009) Spectral properties of simulated impact glasses produced from Martian soil analogue JSC Mars-1. Icarus: International Journal of Solar System Studies, 202 (1), Seiten 336-353. ELSEVIER. DOI: 10.1016/j.icarus.2009.02.007.

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To simulate the formation of impact glasses on Mars, an analogue of martian bright soil (altered volcanic soil JSC Mars-1) was melted at relevant oxygen fugacities using a pulsed laser and a resistance furnace. Reduction of Fe3+ to Fe2+ and in some cases formation of nanophase Fe0 in the glasses were documented by Mössbauer spectroscopy and TEM studies. Reflectance spectra for several size fractions of the JSC Mars-1 sample and the glasses were acquired between 0.3 and 25 μm. The glasses produced from the JSC Mars-1 soil show significant spectral variability depending on the method of production and the cooling rate. In general, they are dark and less red in the visible compared to the original JSC Mars-1 soil. Their spectra do not have absorption bands due to bound water and structural OH, have positive spectral slopes in the near-infrared range, and show two broad bands centered near 1.05 and 1.9 μm, typical of glasses rich in ferrous iron. The latter bands and low albedo partly mimic the spectral properties of martian dark regions, and may easily be confused with mafic materials containing olivine and low-Ca pyroxene. Due to their disordered structures and vesicular textures, the glasses show relatively weak absorption features from the visible to the thermal infrared. These weak absorption bands may be masked by the stronger bands of mafic minerals. Positive near-infrared spectral slopes typical of fresh iron-bearing impact or volcanic glasses may be masked either by oxide/dust coatings or by aerosols in the Mars' atmosphere. As a result, impact glasses may be present on the surface of Mars in significant quantities that have been either misidentified as other phases or masked by phases with stronger infrared features. Spectrometers with sufficient spatial resolution and wavelength coverage may detect impact glasses at certain locations, e.g., in the vicinity of fresh impact craters. Such dark materials are usually interpreted as accumulations of mafic volcanic sand, but the possibility of an impact melt origin of such materials also should be considered. In addition, our data suggest that high contents of feldspars or zeolites are not necessary to produce the transparency feature at 12.1 μm typical of martian dust spectra.

Titel:Spectral properties of simulated impact glasses produced from Martian soil analogue JSC Mars-1
AutorenInstitution oder E-Mail-Adresse der Autoren
Moroz, L.V.Ljuba.moroz@dlr.de
Basilevsky , A.T.Vernadsky Institute, RAS, Moscow, Russia
Hiroi, T.Department of Geological Sciences, Brown University, Providence, RI, USA
Rout, S.S.Institute of Planetology, University of Münster, Münster, Germany
van der Bogert, C.H.Institute of Planetology, University of Münster, Münster, Germany
Yakovlev, O.I.Vernadsky Institute, RAS, Moscow, Russia
Fisenko, A.V.Vernadsky Institute, RAS, Moscow, Russia
Semjonova, L.F.Vernadsky Institute, RAS, Moscow, Russia
Rusakov, V.S.Department of Physics, Moscow State University, Moscow, Russia
Khramov, D.A.Vernadsky Institute, RAS, Moscow, Russia
Zinovieva, N.G.Department of Geology, Moscow State University, Moscow, Russia
Arnold, G.gabriele.arnold@dlr.de
Pieters, C.M.Department of Geological Sciences, Brown University, Providence, RI, USA
Datum:Juli 2009
Erschienen in:Icarus: International Journal of Solar System Studies
Referierte Publikation:Ja
In Open Access:Nein
In ISI Web of Science:Ja
DOI :10.1016/j.icarus.2009.02.007
Seitenbereich:Seiten 336-353
Stichwörter:Mars, surface; Spectroscopy; impact processes; Regoliths
HGF - Forschungsbereich:Verkehr und Weltraum (alt)
HGF - Programm:Weltraum (alt)
HGF - Programmthema:W - keine Zuordnung
DLR - Schwerpunkt:Weltraum
DLR - Forschungsgebiet:W - keine Zuordnung
DLR - Teilgebiet (Projekt, Vorhaben):W -- keine Zuordnung (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Terahertz- und Infrarotsensorik
Hinterlegt von: Dr. Liubov Moroz
Hinterlegt am:06 Jan 2011 13:18
Letzte Änderung:20 Mär 2013 19:43

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