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Near infrared spectroscopy of HED meteorites: Effects of viewing geometry and compositional variations

Ruesch, O. and Hiesinger, H. and Cloutis, E. and Le Corre, Lucille and Kallisch, J. and Mann, P. and Markus, K. and Metzler, K. and Nathues, A. and Reddy, V. (2015) Near infrared spectroscopy of HED meteorites: Effects of viewing geometry and compositional variations. Icarus, 258, pp. 384-401. Elsevier. DOI: 10.1016/j.icarus.2015.06.034 ISSN 0019-1035

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Official URL: http://dx.doi.org/10.1016/j.icarus.2015.06.034

Abstract

The howardite, eucrite and diogenite (HED) meteorites are genetically related and represent the most voluminous group of achondrites. They are the closest analog materials to Vesta and V-type asteroids. Many of these meteorites were the focus of intense petrologic and visible to near infrared spectral studies. As ground-based and orbital observations of basaltic asteroids have increased, an improved understanding of HEDs is needed. For this study, we investigated 24 HED samples, mainly new finds from Northwest Africa (NWA). Visible to near infrared (up to 2.5 μm) spectral measurements under varying illumination and observation geometries were acquired for 4 samples. Phase reddening and bluing (i.e., increase and decrease in spectral slope) is observed for the visible slope as phase angle increase. Monotonic phase reddening can occur for the near infrared slope as phase angle increase. Non-systematic changes with phase angle are found for the Band Area Ratio parameter. At phase angles higher than ∼60°, the decrease of reflectance and decrease of pyroxene bands depth are undistinguishable from admixture of low albedo material to HED samples. To assess the precision of empirical equations relating spectral properties and composition, the pyroxenes, feldspar, and olivine chemistry of the samples was determined. Using previous calibrations, systematic overestimations of the ferrosilite (Fs) and wollastonite (Wo) contents are found, especially in the 15–40 Fs range. To overcome such discrepancies, a new set of empirical equations is proposed. For an application of the new calibration, we selected two compositional end-member areas on Vesta on the basis of their iron content. For the iron-poor terrain we found an average pyroxene composition of Fs30Wo5 and for the iron-rich terrain an average of Fs47Wo14.

Item URL in elib:https://elib.dlr.de/101413/
Document Type:Article
Title:Near infrared spectroscopy of HED meteorites: Effects of viewing geometry and compositional variations
Authors:
AuthorsInstitution or Email of AuthorsAuthors ORCID iD
Ruesch, O.Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, GermanyUNSPECIFIED
Hiesinger, H.Westfälische Wilhelms-Universität MünsterUNSPECIFIED
Cloutis, E.University of Winnipeg, Winnipeg, CanadaUNSPECIFIED
Le Corre, LucillePlanetary Science Institute, Tucson, AZ 85719, USAUNSPECIFIED
Kallisch, J.Westfälische Wilhelms-Universität MünsterUNSPECIFIED
Mann, P.University of Winnipeg, Winnipeg, CanadaUNSPECIFIED
Markus, K.Kathrin.Markus (at) dlr.deUNSPECIFIED
Metzler, K.Westfälische Wilhelms-Universität MünsterUNSPECIFIED
Nathues, A.Max-Planck Institute for Solar System Research, Katlenburg-Lindau, GermanyUNSPECIFIED
Reddy, V.Planetary Science Institute, Tucson, AZ 85719, USAUNSPECIFIED
Date:29 June 2015
Journal or Publication Title:Icarus
Refereed publication:Yes
Open Access:No
Gold Open Access:No
In SCOPUS:Yes
In ISI Web of Science:Yes
Volume:258
DOI :10.1016/j.icarus.2015.06.034
Page Range:pp. 384-401
Publisher:Elsevier
ISSN:0019-1035
Status:Published
Keywords:Meteorites; Spectroscopy; Asteroid Vesta
HGF - Research field:Aeronautics, Space and Transport
HGF - Program:Space
HGF - Program Themes:Space Science and Exploration
DLR - Research area:Raumfahrt
DLR - Program:R EW - Erforschung des Weltraums
DLR - Research theme (Project):R - Projekt ROSETTA Instrumente
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Leitungsbereich PF
Deposited By: Kappel, David
Deposited On:07 Jan 2016 08:29
Last Modified:06 Sep 2019 15:26

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