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Mid-infrared spectral variability for compositionally similar asteroids: Implications for asteroid particle size distributions

Vernazza, P. und Carry, B. und Emery, J. und Hora, J.L. und Cruikshank, D. und Binzel, R.P. und Jackson, J. und Helbert, J. und Maturilli, A. (2010) Mid-infrared spectral variability for compositionally similar asteroids: Implications for asteroid particle size distributions. Icarus: International Journal of Solar System Studies, 207 (2), Seiten 800-809. Elsevier. DOI: 10.1016/j.icarus.2010.01.011.

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Offizielle URL: http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WGF-4Y6S7PT-3&_user=100058&_coverDate=06%2F30%2F2010&_rdoc=1&_fmt=high&_orig=search&_origin=search&_sort=d&_docanchor=&view=c&_acct=C000007338&_version=1&_urlVersion=0&_userid=100058&md5=6dbf6d7fa

Kurzfassung

We report an unexpected variability among mid-infrared spectra (IRTF and Spitzer data) of eight S-type asteroids for which all other remote sensing interpretations (e.g. VNIR spectroscopy, albedo) yield similar compositions. Compositional fitting making use of their mid-IR spectra only yields surprising alternative conclusions: (1) these objects are not â��compositionally similarâ�� as the inferred abundances of their main surface minerals (olivine and pyroxene) differ from one another by 35% and (2) carbonaceous chondrite and ordinary chondrite meteorites provide an equally good match to each asteroid spectrum. Following the laboratory work of Ramsey and Christensen (Ramsey, M.S., Christensen, P.R. [1998]. J. Geophys. Res. 103, 577â��596), we interpret this variability to be physically caused by differences in surface particle size and/or the effect of space weathering processes. Our results suggest that the observed asteroids must be covered with very fine (<5 �¼m) dust that masks some major and most minor spectral features. We speculate that the compositional analysis may be improved with a spectral library containing a wide variety of well characterized spectra (e.g., olivine, orthopyroxene, feldspar, iron, etc.) obtained from very fine powders. In addition to the grain size effect, space weathering processes may contribute as well to the reduction of the spectral contrast. This can be directly tested via new laboratory irradiation experiments.

Dokumentart:Zeitschriftenbeitrag
Titel:Mid-infrared spectral variability for compositionally similar asteroids: Implications for asteroid particle size distributions
Autoren:
AutorenInstitution oder E-Mail-Adresse der Autoren
Vernazza, P.Research and Scientific Support Department, European Space Agency, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
Carry, B.Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, 5 Place Jules Janssen, Meudon F-92195, France
Emery, J.Department of Earth and Planetary Sciences, Knoxville, TN 37996-1410, USA
Hora, J.L.Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
Cruikshank, D.NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035, USA
Binzel, R.P.NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035, USA
Jackson, J.Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA
Helbert, J.Joern.Helbert@dlr.de
Maturilli, A.Alessandro.Maturilli@dlr.de
Datum:Juni 2010
Erschienen in:Icarus: International Journal of Solar System Studies
Referierte Publikation:Ja
In Open Access:Nein
In SCOPUS:Ja
In ISI Web of Science:Ja
Band:207
DOI :10.1016/j.icarus.2010.01.011
Seitenbereich:Seiten 800-809
Verlag:Elsevier
Status:veröffentlicht
Stichwörter:Asteroids; Surfaces; Spectroscopy; Mineralogy; Meteorites
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 Asteroiden und Kometen (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Terahertz- und Infrarotsensorik
Hinterlegt von: Alessandro Maturilli
Hinterlegt am:11 Jan 2011 15:03
Letzte Änderung:12 Dez 2013 21:12

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