Spectral evidence for amorphous silicates in least-processed CO meteorites and their parent bodies

1,2Margaret M. McAdam, 1Jessica M. Sunshine, 3,4Kieren T. Howard, 5Conel M. Alexander, 6Timothy J. McCoy, 7Schelte J. Bus
Icarus 306, 32-49 Link to Article [https://doi.org/10.1016/j.icarus.2018.01.024]
1University of Maryland, Department of Astronomy, College Park, MD 20740, USA
2Northern Arizona University, Department of Physics and Astronomy, Flagstaff AZ 86011, USA
3American Museum of Natural History, Central Park West & 79th St, New York, NY 10024, USA
4Kingsborough Community College, 2001 Oriental Blvd, Brooklyn, NY 11235, USA
5Department of Terrestrial Magnetism, Carnegie Institution, 1530 P St NW, Washington, DC 20005, USA
6National Museum of Natural History, Smithsonian Institution, 600 Maryland Avenue SW, Washington, DC 20002, USA
17University of Hawaii, Institute for Astronomy, 2444 Dole St, Honolulu, HI 96822, USA
Copyright Elsevier

Least-processed carbonaceous chondrites (carbonaceous chondrites that have experienced minimal aqueous alteration and thermal metamorphism) are characterized by their predominately amorphous iron-rich silicate interchondrule matrices and chondrule rims. This material is highly susceptible to destruction by the parent body processes of thermal metamorphism or aqueous alteration. The presence of abundant amorphous material in a meteorite indicates that the parent body, or at least a region of the parent body, experienced minimal processing since the time of accretion. The CO chemical group of carbonaceous chondrites has a significant number of these least-processed samples. We present visible/near-infrared and mid-infrared spectra of eight least-processed CO meteorites (petrologic type 3.0–3.1). In the visible/near-infrared, these COs are characterized by a broad weak feature that was first observed by Cloutis et al. (2012) to be at 1.3-µm and attributed to iron-rich amorphous silicate matrix materials. This feature is observed to be centered at 1.4-µm for terrestrially unweathered, least-processed CO meteorites. At mid-infrared wavelengths, a 21-µm feature, consistent with Si–O vibrations of amorphous materials and glasses, is also present. The spectral features of iron-rich amorphous silicate matrix are absent in both the near- and mid-infrared spectra of higher metamorphic grade COs because this material has recrystallized as crystalline olivine. Furthermore, spectra of least-processed primitive meteorites from other chemical groups (CRs, MET 00426 and QUE 99177, and C2-ungrouped Acfer 094), also exhibit a 21-µm feature. Thus, we conclude that the 1.4- and 21-µm features are characteristic of primitive least-processed meteorites from all chemical groups of carbonaceous chondrites. Finally, we present an IRTF + SPeX observation of asteroid (93) Minerva that has spectral similarities in the visible/near-infrared to the least-processed CO carbonaceous chondrites. While Minerva is not the only CO-like asteroid (e.g., Burbine et al., 2001), Minerva is likely the least-processed CO-like asteroid observed to date.


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