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Constraints on Mercury’s surface composition from MESSENGER and ground-based spectroscopy

Warell, J. und Sprague, A. und Kozlowski, R. und Rothery, D.A. und Lewis, N. und Helbert, J. und Cloutis, E. (2010) Constraints on Mercury’s surface composition from MESSENGER and ground-based spectroscopy. Icarus: International Journal of Solar System Studies, 209 (1), Seiten 138-163. ELSEVIER. DOI: 10.1016/j.icarus.2010.04.008

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The composition and chemistry of Mercury’s regolith has been calculated from MESSENGER MASCS 0.3–1.3 μm spectra from the first flyby, using an implementation of Hapke’s radiative transfer-based photometric model for light scattering in semi-transparent porous media, and a linear spectral mixing algorithm. We combine this investigation with linear spectral fitting results from mid-infrared spectra and compare derived oxide abundances with mercurian formation models and lunar samples. Hapke modeling results indicate a regolith that is optically dominated by finely comminuted particles with average area weighted grain size near 20 μm. Mercury shows lunar-style space weathering, with maturation-produced microphase iron present at ˜0.065 wt.% abundance, with only small variations between mature and immature sites, the amount of which is unable to explain Mercury’s low brightness relative to the Moon. The average modal mineralogies for the flyby 1 spectra derived from Hapke modeling are 35–70% Na-rich plagioclase or orthoclase, up to 30% Mg-rich clinopyroxene, <5% Mg-rich orthopyroxene, minute olivine, ˜20–45% low-Fe, low-Ti agglutinitic glass, and <10% of one or more lunar-like opaque minerals. Mercurian average oxide abundances derived from Hapke models and mid-infrared linear fitting include 40–50 wt.% SiO2, 10–35 wt.% Al2O3, 1–8 wt.% FeO, and <25 wt.% TiO2; the inferred rock type is basalt. Lunar-like opaques or glasses with high Fe and/or Ti abundances cannot on their own, or in combination, explain Mercury’s low brightness. The linear mixing results indicate the presence of clinopyroxenes that contain up to 21 wt.% MnO and the presence of a Mn-rich hedenbergite. Mn in M1 crystalline lattice sites of hedenbergite suppresses the strong 1 and 2 μm crystal field absorption bands and may thus act as a strong darkening agent on Mercury. Also, one or more of thermally darkened silicates, Fe-poor opaques and matured glasses, or Mercury-unique Ostwald-ripened microphase iron nickel may lower the albedo. A major part of the total microphase iron present in Mercury’s regolith is likely derived from FeO that is not intrinsic to the crust but has been subsequently delivered by exogenic sources.

Titel:Constraints on Mercury’s surface composition from MESSENGER and ground-based spectroscopy
AutorenInstitution oder E-Mail-AdresseAutoren-ORCID
Warell, J.Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, SwedenNICHT SPEZIFIZIERT
Sprague, A.Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721-0091, USANICHT SPEZIFIZIERT
Kozlowski, R. Department of Physics, Susquehanna University, 514 University Avenue, Selinsgrove, PA 17870, USANICHT SPEZIFIZIERT
Rothery, D.A.Department of Earth and Environmental Sciences, The Open University, Milton Keynes MK7 6AA, UKNICHT SPEZIFIZIERT
Lewis, N.Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721-0091, USANICHT SPEZIFIZIERT
Helbert, J. joern.helbert@dlr.deNICHT SPEZIFIZIERT
Cloutis, E.Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba, CanadaNICHT SPEZIFIZIERT
Datum:September 2010
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.2010.04.008
Seitenbereich:Seiten 138-163
Stichwörter:Mercury, Surface; Mineralogy; Radiative transfer; Regoliths; Spectroscopy
HGF - Forschungsbereich:Verkehr und Weltraum (alt)
HGF - Programm:Weltraum (alt)
HGF - Programmthema:W EW - Erforschung des Weltraums
DLR - Schwerpunkt:Weltraum
DLR - Forschungsgebiet:W EW - Erforschung des Weltraums
DLR - Teilgebiet (Projekt, Vorhaben):W - Vorhaben BepiColombo (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Terahertz- und Infrarotsensorik
Hinterlegt von: Stiebeler, Ulrike
Hinterlegt am:12 Jan 2011 10:40
Letzte Änderung:18 Jul 2014 00:20

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