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Mercury: Mg-rich mineralogy with K-spar and garnet

Sprague, A. L. und Donaldson, K. L. und Kozlowski, R.W.H. und Helbert, J. und Maturilli, A. und Izenberg, N. R. (2008) Mercury: Mg-rich mineralogy with K-spar and garnet. In: Lunar and Planetary Science XXXIX, 1391, abstract#1320. Lunar and Planetary Institute, Houston, TX. 39th Lunar and Planetary Science Conference, 2008-03-10 - 2008-03-14, Houston, TX (USA). ISSN 1540-7845

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Offizielle URL: http://www.lpi.usra.edu/meetings/lpsc2008/pdf/1320.pdf


<p>Introduction: We report the results of spectral unmixing at two distinct regions near the footprint of the 1st flyby of Mercury by the MESSENGER spacecraft. Results indicate that both regions have Mg-rich chemistry, K-spar, and the presence of minor Ca-and Mg-rich garnets. However, one region is more mafic (primarily enstatite) than the other (primarily labradorite). Labradorite, orthopyroxene [1], and clinopyroxene [2,3] have previously been identified at other locations on Mercury’s surface. This is the first time that many spectra from the same locations on Mercury have been analyzed by spectral unmixing using a welldocumented deconvolution algorithm [4,5].</p><p> Observations: Mid-infrared 2-D long-slit spectral imaging from 8.2 to 12.7 μm of Mercury was obtained during daytime observations 7-8 April 2006. At the time of the observations, Mercury was between ~7.8 arc seconds in diameter, 0.46 AU from the Sun, with the sub-Earth longitude varying from 172° to 196°W. longitude. We used MIRSI’s 10-μm grism covering 8 - 14 μm with λ/Δλ equal to 200 and a slit width of 0.6″ in chop/nod mode. The MIRSI detector is a 16-channel 320 x 240 Si:As IBC array developed by Raytheon; each channel measures 20 x 240 pixels [6]. To position the slit over the desired location, we obtained 7.7 μm filter images just prior to each spectral image. Spectral images of β Pegasus just prior to and following Mercury observations were used as our standard calibrator. Spectra were corrected for telluric effects and ratioed to rough surface thermal models computed for the time of observation to remove the blackbody continuum. Fig. 1 gives the locations of observations as regions within red rectangles and in proximity to the M1 flyby footprint.</p><p> Spectral Deconvolution and Mineral Identification: These data are the first Mercury data to be compositionally analyzed by a spectral deconvolution, or spectral unmixing, technique. Inputs into the spectral deconvolution algorithm [3] include the data spectrum to be unmixed and the end member spectral library of minerals measured at the same wavelengths as the unmixed data spectrum. Results of a blind retrieval test where spectral end members were known to be in the spectral library showed that for each mineral in the mixture differences between the unmix model abundance and the actual abundance was between 4 and 12%. More recently linear deconvolution of plagioclase feldspar sands using the same deconvolution algorithm demonstrated the success of determining the proper feldspar composition to within 5% modal anorthite for compositionally complex mixtures [4].</p><p> Spectral libraries: In our case we do not have known end member spectra and uncertainties are not so well quantified. The quality of the spectral library is critically important and we have found that spectral libraries with a range of small grain sizes are essential for matching Mercury spectra. Thus, we have built mid-infrared spectral libraries using laboratory spectra from a wide range of sources (USGS, RELAB, BED, JHU, JPL, ASU). We used spectra of minerals typical in lunar soils and terrestrial basalts, trachytes, and other rocks of magmatic origin but were unable to find adequate compositional variety in clinopyroxenes. We added spectra of garnet to the end-member libraries because no good fit could be obtained until pyrope and grossular were available in the end member library for unmixing.</p><p> Results: Hundreds of unmixing models were run restricting endmember compositions until we had repeated good fits. To illustrate the uncertainty in the “best-fit” models we show alternative fits with high (sanadine) and low (orthoclase) temperature K-spar in Fig. 3 (122°E, 238°W) and Fig. 4 (150°E, 210°W). Also shown is the difference between a fit using forsterite, which gives the best fit, vs. fayalite for olivine (Fig. 3) and labradorite, which gives the best fit vs. bytownite (Fig. 4).</p>

Dokumentart:Konferenzbeitrag (Poster)
Titel:Mercury: Mg-rich mineralogy with K-spar and garnet
AutorenInstitution oder E-Mail-AdresseAutoren-ORCID
Sprague, A. L.Lunar and Planetary Laboratory, Tucson, AZ 85721NICHT SPEZIFIZIERT
Donaldson, K. L.Lunar and Planetary Laboratory, Tucson, AZ 85721NICHT SPEZIFIZIERT
Kozlowski, R.W.H.Susquehanna University, Selinsgrove, PA, 17870NICHT SPEZIFIZIERT
Izenberg, N. R.Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723NICHT SPEZIFIZIERT
Datum:März 2008
Erschienen in:Lunar and Planetary Science XXXIX
Referierte Publikation:Ja
In Open Access:Nein
In ISI Web of Science:Nein
Verlag:Lunar and Planetary Institute, Houston, TX
Name der Reihe:LPI Contribution
Stichwörter:Mercury; MESSENGER; feldspars; K-rich; Mg-rich; garnet; Mid-infrared; MIRSI; Spectral deconvolution
Veranstaltungstitel:39th Lunar and Planetary Science Conference
Veranstaltungsort:Houston, TX (USA)
Veranstaltungsart:internationale Konferenz
Veranstaltungsdatum:2008-03-10 - 2008-03-14
Veranstalter :Lunar and Planetary Institute
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 Vergleichende Planetologie (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Planetenphysik
Hinterlegt von: Hempel, Stefanie
Hinterlegt am:30 Apr 2008
Letzte Änderung:27 Apr 2009 14:54

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