Meteorites Acfer

Pedroni, A., Begemann, F. (1994) On unfractionated solar gases in the H3-6 meteorite Acfer 111. Meteoritics, 29, 632-42. 

Sugiura, N. and Krot, A.N. (2007) 26Al-26Mg systematics of Ca-Al-rich inclusions, amoeboid olivine aggregates and chondrules form the ungrouped carbonaceous chondrite Acfer 094. Meteoritics and Planetary Science, 42, 1183-1195. 

Grady, M. M. Pillinger, C. T. 1992 The continuing search for the location of 15N-enriched nitrogen in Acfer 182. Meteoritics 27, 226-227. 

Figure 2.5 Presolar grains from primitive meteorites. Left presolar SiC from the Murchison meteorite scale bar is 200 nm. Middle presolar graphite from Murchison scale bar is 1 pm. Right presolar silicate grain (within the white circle) in the matrix of the Acfer 094 meteorite scale bar is 500 nm. Photo credit Max Planck Institute for Chemistry.

Messenger S. and Bernatowicz T. J. (2000) Search for presolar silicates in Acfer 094. Meteorit. Planet. Sci. 35, A109. 

Newton J., Bischoff A., Arden J. W., Franchi I. A., Geiger T., Greshake A., and Pillinger C. T. (1995) Acfer 094, a uniquely primitive carbonaceous chondrite from the Sagara. Meteoritics 30, 47-56. 

Bischolf et al. (1993) first proposed the name CH for a small group of very metal-rich chondrites that otherwise are chemically and mineralogically similar to the CR chondrites. The best-studied CH meteorites are ALH85085 (and several similar Antarctic meteorites) and Acfer 182. The two are chemically similar but the components in Acfer 182 are, on average, larger than those in ALH85085. 

The CAI population in CH meteorites is distinctive in several respects relative to other chondrites. First, the CAIs are very small. The largest CAI reported in Acfer 182 is 450 p,m in size and most are less than 300 p,m (Weber et al., 1995) ... 

Sahijpal S., McKeegan K. D., Krot A. N., Weber D., and Ulyanov A. A. (1999) Oxygen isotopic compositions of Ca—Al-rich inclusions from the CH chondrites, Acfer 182 and Pat91546. Meteorit Planet Sci. 34, AlOl. 

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