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Vesta’s mineralogical composition as as revealed by the visible and infrared spectrometer on Dawn

Desanctis, M.C. and Ammannito, E. and Capria, M. T. and Combe, J. P. and Frigeri, A. and Longobardo, A and Magni, G. and Marchi, S. and McCord, T. B. and Palomba, E. and Tosi, F. and Zambon, F. and Carraro, F. and Fonte, S. and Li, Y. J. and McFadden, L.A. and Mittlefehldt, D. W. and Pieters, C. and Jaumann, R. and Stephan, K. and Raymond, C.A. and Russell, C.T. (2013) Vesta’s mineralogical composition as as revealed by the visible and infrared spectrometer on Dawn. Meteoritics & Planetary Science, 48 (11), pp. 2166-2184. Wiley. DOI: 10.1111/maps.12138 ISSN 1086-9379

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Official URL: http://onlinelibrary.wiley.com/doi/10.1111/maps.12138/abstract

Abstract

The Dawn spacecraft mission has provided extensive new and detailed data on Vesta that confirm and strengthen the Vesta–howardite–eucrite–diogenite (HED) meteorite link and the concept that Vesta is differentiated, as derived from earlier telescopic observations. Here, we present results derived by newly calibrated spectra of Vesta. The comparison between data from the Dawn imaging spectrometer—VIR—and the different class of HED meteorites shows that average spectrum of Vesta resembles howardite spectra. Nevertheless, the Vesta spectra at high spatial resolution reveal variations in the distribution of HED-like mineralogies on the asteroid. The data have been used to derive HED distribution on Vesta, reported in Ammannito et al. (2013), and to compute the average Vestan spectra of the different HED lithologies, reported here. The spectra indicate that, not only are all the different HED lithologies present on Vesta, but also carbonaceous chondritic material, which constitutes the most abundant inclusion type found in howardites, is widespread. However, the hydration feature used to identify carbonaceous chondrite material varies significantly on Vesta, revealing different band shapes. The characteristic of these hydration features cannot be explained solely by infalling of carbonaceous chondrite meteorites and other possible origins must be considered. The relative proportion of HEDs on Vesta's surface is computed, and results show that most of the vestan surface is compatible with eucrite-rich howardites and/or cumulate or polymict eucrites. A very small percentage of surface is covered by diogenite, and basaltic eucrite terrains are relatively few compared with the abundance of basaltic eucrites in the HED suite. The largest abundance of diogenitic material is found in the Rheasilvia region, a deep basin, where it clearly occurs below a basaltic upper crust. However, diogenite is also found elsewhere; although the depth to diogenite is consistent with one magma ocean model, its lateral extent is not well constrained.

Item URL in elib:https://elib.dlr.de/84028/
Document Type:Article
Title:Vesta’s mineralogical composition as as revealed by the visible and infrared spectrometer on Dawn
Authors:
AuthorsInstitution or Email of AuthorsAuthors ORCID iD
Desanctis, M.C.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIED
Ammannito, E.INAF, Istituto di Fisica Dello Spazio Interplanetario, Roma, ItalyUNSPECIFIED
Capria, M. T.Instituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIED
Combe, J. P.Space Science Inst., Winthrop WA, USA, Lab. de Planetologie et de Geodynamique, U. de Nantes, Nantes, FranceUNSPECIFIED
Frigeri, A.National Institute of Astrophysics, Rome, ItalyUNSPECIFIED
Longobardo, AINAF-LAPS, Via del Fosso del Cavaliere 100, I-00133 Rome, ItalyUNSPECIFIED
Magni, G.INAF/Instituto di Astrofisica Spaziale e Fisica Cosmica, Rome, ItalyUNSPECIFIED
Marchi, S.Department of Astronomy, University of PaduaUNSPECIFIED
McCord, T. B.HIGP/SOEST, University of Hawaii, Winthrop, WA, USAUNSPECIFIED
Palomba, E.Institute for Interplanetary Space Physics - INAF, Rome, ItalyUNSPECIFIED
Tosi, F.INAF-IASF Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma ItalyUNSPECIFIED
Zambon, F.INAF-IAPS, Via del Fosso del Cavaliere 100, I-00133 Rome, ItalyUNSPECIFIED
Carraro, F.INAF/Instituto di Fisica dello Spazio Interplanetarario, Rome, ItalyUNSPECIFIED
Fonte, S.INAF/Instituto di Fisica dello Spazio Interplanetarario, Rome, ItalyUNSPECIFIED
Li, Y. J.Planetary Science Institute, Tucson, Arizona, 85719, USAUNSPECIFIED
McFadden, L.A.University of Maryland, College Park, MD, USAUNSPECIFIED
Mittlefehldt, D. W.Astromaterials Research Office, NASA Johnson Space Center, Houston, Texas, USAUNSPECIFIED
Pieters, C.Brown University, Providence, RI, USAUNSPECIFIED
Jaumann, R.ralf.jaumann (at) dlr.deUNSPECIFIED
Stephan, K.katrin.stephan (at) dlr.deUNSPECIFIED
Raymond, C.A.Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USAUNSPECIFIED
Russell, C.T.Institute of Geophysics, University of California, Los Angeles, Los Angeles, CA 90095UNSPECIFIED
Date:8 July 2013
Journal or Publication Title:Meteoritics & Planetary Science
Refereed publication:Yes
In SCOPUS:Yes
In ISI Web of Science:Yes
Volume:48
DOI :10.1111/maps.12138
Page Range:pp. 2166-2184
Publisher:Wiley
ISSN:1086-9379
Status:Published
Keywords:DAWN, Vesta, mineralogical compositionas, infrared spectrometer
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 DAWN
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Geology
Deposited By: Voigt, Joana
Deposited On:18 Sep 2013 11:03
Last Modified:08 Mar 2018 18:53

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