Meteoritics & Planetary Science 41, Nr 8, Supplement, A13–A199 (2006) http://meteoritics.org Abstracts 5367 5372 CHARACTERIZATION OF ASTEROIDAL BASALTS THROUGH ONSET OF AQUEOUS ALTERATION IN PRIMITIVE CR REFLECTANCE SPECTROSCOPY AND IMPLICATIONS FOR THE CHONDRITES DAWN MISSION N. M. Abreu and A. J. Brearley. Department of Earth and Planetary Sciences, P. A. Abell 1, D. W. Mittlefehldt1, and M. J. Gaffey2. 1Astromaterials Research University of New Mexico, Albuquerque, New Mexico 87131, USA. E-mail: and Exploration Science, NASA Johnson Space Center, Houston, Texas
[email protected] 77058, USA. 2Department of Space Studies, University of North Dakota, Grand Forks, North Dakota 58202, USA Introduction: Although some CR chondrites show evidence of significant aqueous alteration [1], our studies [2] have identified CR Introduction: There are currently five known groups of basaltic chondrites that exhibit only minimal degrees of aqueous alteration. These achondrites that represent material from distinct differentiated parent bodies. meteorites have the potential to provide insights into the earliest stages of These are the howardite-eucrite-diogenite (HED) clan, mesosiderite silicates, aqueous alteration and the characteristics of organic material that has not angrites, Ibitira, and Northwest Africa (NWA) 011 [1]. Spectroscopically, all been affected by aqueous alteration, i.e., contains a relatively pristine record these basaltic achondrite groups have absorption bands located near 1 and 2 of carbonaceous material present in nebular dust. The CR chondrites are of microns due to the presence of pyroxene. Some of these meteorite types have special significance in this regard, because they contain the most primitive spectra that are quite similar, but nevertheless have characteristics (e.g., carbonaceous material currently known [3].