Sample Petrographic Description
Sample Number | MIL 091010 |
Newsletter | 33,2 |
Location | Miller Range |
Field Number | 20249 |
Dimensions (cm) | 3.0 x 2.0 x 5.75 |
Weight (g) | 51.66 |
Original Classification | CV3 Chondrite |
Updated Classification | CV 3.7 Chondrite Oxidized A |
Pairing | MIL 07590; MIL 07002; MIL 07385; MIL 07403; MIL 07669; MIL 07671; MIL 07678; MIL 07681; MIL 07683; MIL 07684; MIL 07685; MIL 07686; MIL 07690; MIL 07691; MIL 07694; MIL 07696; MIL 07698; MIL 07699; MIL 090072; MIL 090170; MIL 090171; MIL 090172; MIL 090173; MIL 090174; MIL 090175; MIL 090176; MIL 090177; MIL 090178; MIL 090179; MIL 090184; MIL 091010; MIL 11206; MIL 15306; |
Mineral Composition (%Fa & %Fs) | |
Fayalite (mol%): 0-41;Ferrosilite (mol%): 1 | |
Weathering | |
B | |
Fracturing | |
B | |
Macroscopic Description - Roger Harrington, Kathleen McBride | |
30% to 50% of the exteriors of these meteorites are covered with dull black fusion crust. The remaining broken surfaces consists of dark gray fine-grained matrix with 1-2 mm CAI’s scattered throughout. The interiors of these samples are dark to medium gray, fine grained matrix with visible chondrules and numerous 1-2 mm light gray CAI’s. | |
Thin Section Description (,2) - Cari Corrigan, Linda Welzenbach | |
The sections are so similar that a single description suffices. The sections exhibit large chondrules (up to 3 mm) and CAIs in a dark matrix. Olivines range from Fa0-43 and low-Ca pyroxene is Fs0-1. The meteorites are unequilibrated carbonaceous chondrites, probably reduced CV3s. These are likely paired with the MIL 07671 pairing group previously reported. | |
Reclassification Notes (AMN 46,1) | |
Reclassification and pairing based on Raman spectroscopy (petrologic type 3.7), and on Ni content of metal and sulfide and magnetic susceptibility (Oxidized A). Details are reported in Righter et al. (2022); doi: 10.1111/maps.13932. | |
Notes | |
The meteorite was discovered enclosed in blue ice. The meteorite and enclosed ice were collected as a coherent block and transported to JSC that way, and kept in JSC freezers until April 2010. Ice and meteorite were then transported to the Cold Region Research and Engineering Laboratory (CRREL) in Hanover NH, for extraction of meteorite from the ice using cold room equipment. After removal, the meteorite was transported back to Houston, still frozen, and introduced into the Meteorite Processing Lab. It was thawed and characterized following the standard procedures for the lab, and, of course, is available for study. Samples of the enclosed ice may be available for additional studies if there is interest – please inquire with the JSC Antarctic Meteorite Curation group. |
Antarctic Meteorite Images for Sample MIL 091010 | ||||
Lab Photo(s) : | ||||
Antarctic Meteorite Images for Sample MIL 091010 | ||||
Thin Section Photo(s) : | ||||
References for Sample MIL091010 | |
Eschrig, J., Bonal, L., Beck, P., Prestgard, T.J., 2021, Spectral reflectance analysis of type 3 carbonaceous chondrites and search for their asteroidal parent bodies. Icarus, 354, 114034, https://doi.org/10.1016/j.icarus.2020.114034. | |
Bonal, L., Gattacceca, J., Garenne, A., Eschrig, J., Rochette, P., and Ruggiu, L.K., 2020, Water and heat: New constraints on the evolution of the CV chondrite parent body. Geochimica et Cosmochimica Acta, 276, 363–383. | |
Gattacceca, J., Bonal, L., Sonzogni, C., and Longerey, J., 2020, CV Chondrites: More than one parent body. Earth and Planetary Science Letters, 547, 116467, doi: 10.1016/j.epsi2020.116467. | |
Bonal, L., Quirico, E., Flandinet, L., Montagnac, G., 2016, Thermal history of type 3 chondrites from the Antarctic meteorite collection determined by Raman spectroscopy of their polyaromatic carbonaceous matter. Geochimica et Cosmochimica Acta, 189, 312-337. |