Shergotty; Zagami; EETA79001; QUE94201; Dar al Gani 476, 489, 670, 735, 876, 975, and 1037;
Yamato 980459; Los Angeles 001 and 002; Sayh al Uhaymir 005, 008, 051, 060, 090, 094, 120, 125, 130, 131, 150;
Dhofar 019 and 378; Northwest Africa 480, 856, 1068, 1110, 1195, 1460, 1669, 1775 and 2046

The martian meteorites most readily available for study are the large basaltic shergottites Zagami (various sources) and EETA79001 (MWG). Shergotty and QUE94201 have been of limited availability. The other samples referred to above are relatively new finds.

The basaltic shergottites are pyroxene-plagioclase igneous rocks in which the plagioclase has been converted to maskelynite glass by shock. Pyroxenes are mostly pigeonite and augite. Accessory phases include mesostasis, impact melt, olivine, orthopyroxene, and various oxides, sulfides and phosphates. Igneous textures range from fine to medium grained and two samples contain multiple lithologies. Most of the samples appear to be magmas with excess pyroxene over true liquid compositions. Several of the samples contain evidence of interaction with martian water, either as hydrated silicate minerals or carbonate and sulfate salts.

Bulk major element compositions generally reflect the mineral modes such that those richest in pyroxene have highest Mg and Fe and lowest Al contents. The basalts all have moderately to strongly light rare earth-depleted REE patterns reflecting a fractionated parent liquid. Noble gas analyses of glasses in two basalts show that they contain trapped martian atmosphere.

The basalts all have very young crystallization ages of 160-180 Ma (million years). Most of them have cosmic ray exposure ages of 2.4-2.8 Ma, but EETA79001 has an exposure age of 600 Ka. These meteorites have terrestrial ages varying from 34 years to 12 Ka.