E Group

The chondrites of this group are named for their primary mineral, enstatite, and they differ in many respects from ordinary and carbonaceous chondrites. They must have formed in an oxygen-depleted environment because nearly all of the iron in E chondrites is present in its reduced, metallic form. Even the pyroxene is depleted in iron, and consequently, it is only found as the pure magnesium-rich end-member - enstatite. After taking into consideration all of the possible pairings among the meteorites recovered in the strewn fields of Africa and in Antarctica, approximately 90 different E chondrites have been identified.

Similar to the ordinary chondrites, the enstatite chondrites have been further subdivided based on their content of total iron; members of the EL group contain less iron than members of the EH group. Moreover, there are mineralogical aspects that separate the two groups. The EL chondrites show petrologic types 3 to 7, and there is a distinct peak at the equilibrated type 6. The members of the EH subgroup exhibit petrologic types from 3 to 6 with a less distinct peak at the unequilibrated type 3.

Despite the differences, most researchers believe that both subgroups originated on the same asteroid, most probably representing different layers of the parent body. Some scientists think that we should look for this asteroid inside the orbit of Venus or even Mercury since the E chondrites formed under highly reducing conditions in an oxygen-depleted environment. Other researchers suggest that a formation in the inner asteroid belt would have provided the same conditions in the early solar system. A more recent comparison of the reflectance spectra of different asteroids to the spectrum of the EH chondrite Abee suggests that the main belt asteroid 16 Psyche might be the common parent for the enstatite chondrites.

Sahara 97159 EH3 Year found: Jul 1997, sahara TKW : 300 gr
				Sahara 97159- 00 45 gr Very nice full slice with a terribly beautifull matrix ! Sold