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Mineralogical Mapping of Quadrangle Av-2 (Belicia) and Av-3 (Caparronia) on 4 Vesta.

Stephan, K. und Frigeri, A. und Barucci, M.A. und Sunshine, J. und Jaumann, R. und Palomba, E. und Blewett, D. und Yingst, R. Aileen und Marchi, S. und De sanctis, M.C. und Matz, Klaus-Dieter und Roatsch, Thomas und Preusker, Frank und Le Corre, L. und Reddy, V. und Russell, C.T. und Raymond, C.A. (2012) Mineralogical Mapping of Quadrangle Av-2 (Belicia) and Av-3 (Caparronia) on 4 Vesta. In: Copernicus. EGU 2012, 2012-04-22 - 2012-04-27, Wien, Österreich.

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Kurzfassung

Since the arrival of the Dawn spacecraft at 4 Vesta on July 16, 2011 the Visible and InfraRed Imaging Spectrometer (VIR) has acquired hyperspectral images of Vesta's surface, which enable to characterize Vesta's mineralogical composition in the wavelength range from 0.25 to 5.1µm. As part of the analysis of Vesta's surface composition the science team is preparing a series of 15 quadrangle maps showing the results derived from the spectroscopic analysis of the VIR and FC color data. We present preliminary results of the spectroscopic analysis achieved for the quadrangles Av-2 (Belicia) and Av-3 (Caparronia), which show Vesta's surface between 21°N - 66° N°, 0° - 90°E and 90° - 180° E, respectively. These results are based on the analysis of the combination of the visible albedo, spectral parameters including the position, depth of the pyroxene absorptions, as well as color ratio composites using the VIR channels centering at 749nm/438nm (Red), 749nm/917nm (Green) and 438nm/749nm (Blue). Vesta's rotation axis, however, is tilted ~29° with respect to its orbital plane. Since Dawn arrived during northern winter, portions of Vesta north of ~45° N are dominated by extended shadows or have not yet been imaged due to permanent night. Thus, limited FC color or VIR hyperspectral data have been available for the quadrangles Av-2 and Av-3. The illuminated parts are dominated by a heavily-cratered northern terrain with ancient troughs and grooves and named after the prominent relatively large impact craters Belicia (~37°N/48°E) and Caparronia (~36°N/167°E). Numerous impact craters of different size, morphology, and state of surface degradation are apparent. Most spectral variations are strongly affected by the extreme illumination conditions, making the analysis of albedo variations and spectral signatures rather difficult. Their interpretation thus remains. Nevertheless, VIR spectra show clear evidence of Vesta's surface composition similar to those of HED (howardite, eucrite and diogenite) meteorites. The prominent pyroxene absorptions near 0.9 and 1.9µm show different band depths and band centers, which are associated with the presence and abundance of the mafic minerals as well as grain size. Within the quadrangles Av-2 and Av3, band centers appear to shift slightly to shorter wavelength from W to E following the trend of the equatorial region. A similar trend can be observed with respect to the depth of the pyroxene absorptions with the absorption deepening eastward. Locally, bright material associated with strong pyroxene absorptions is observed on crater walls of a few relatively large impact craters with pronounced topography. Either these impact craters are relatively young or fresh material became exposed due mass wasting processes. The effects of photometry for under these illumination conditions are being assessed. The authors gratefully acknowledge the support of the Dawn Instrument, Operations, and Science Teams. This work is supported by NASA through the Dawn project and the German Space Agency (DLR).

elib-URL des Eintrags:https://elib.dlr.de/80553/
Dokumentart:Konferenzbeitrag (NICHT SPEZIFIZIERT)
Titel:Mineralogical Mapping of Quadrangle Av-2 (Belicia) and Av-3 (Caparronia) on 4 Vesta.
Autoren:
AutorenInstitution oder E-Mail-AdresseAutoren-ORCID-iD
Stephan, K.katrin.stephan (at) dlr.de
Frigeri, A.National Institute of Astrophysics, Rome, Italy
Barucci, M.A.Observatoire de Paris-Meudon, France
Sunshine, J.Uni. of Maryland, College Park, MD, USA
Jaumann, R.ralf.jaumann (at) dlr.de
Palomba, E.Institute for Interplanetary Space Physics - INAF, Rome, Italy
Blewett, D.Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Rd. Laurel, MD 20723-6099, USA
Yingst, R. AileenPlanetary Science Institute, Tucson, AZ, United States.
Marchi, S.Department of Astronomy, University of Padua
De sanctis, M.C.Istituto Nazionale di Astrofisica, Rome, Italy.
Matz, Klaus-Dieterklaus-dieter.matz (at) dlr.dehttps://orcid.org/0000-0002-4148-1926
Roatsch, Thomasthomas.roatsch (at) dlr.de
Preusker, Frankfrank.preusker (at) dlr.dehttps://orcid.org/0000-0001-9005-4202
Le Corre, L.Max Planck Institute for Solar System Research, Max-Planck-Str. 2, Katlenburg-Lindau, 37191, Germany
Reddy, V.Department of Space Studies, University of North Dakota, Grand Forks, ND 58202, USA
Russell, C.T.Institute of Geophysics, University of California, Los Angeles, Los Angeles, CA 90095
Raymond, C.A.Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
Datum:April 2012
Erschienen in:Copernicus
Open Access:Ja
Gold Open Access:Nein
In SCOPUS:Nein
In ISI Web of Science:Nein
Status:veröffentlicht
Stichwörter:Vesta, Dawn, Mineralogy
Veranstaltungstitel:EGU 2012
Veranstaltungsort:Wien, Österreich
Veranstaltungsart:internationale Konferenz
Veranstaltungsbeginn:22 April 2012
Veranstaltungsende:27 April 2012
HGF - Forschungsbereich:Luftfahrt, Raumfahrt und Verkehr
HGF - Programm:Raumfahrt
HGF - Programmthema:Erforschung des Weltraums
DLR - Schwerpunkt:Raumfahrt
DLR - Forschungsgebiet:R EW - Erforschung des Weltraums
DLR - Teilgebiet (Projekt, Vorhaben):R - Projekt DAWN (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Planetengeologie
Hinterlegt von: Aydin, Zeynep
Hinterlegt am:11 Jan 2013 14:06
Letzte Änderung:24 Apr 2024 19:47

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