Mixing models using major and trace elements show that the bulk composition
of lithology A (xenocryst-bearing magnesian basalt) of Elephant Moraine A7
9001 (EETA79001) can be reasonably approximated as a simple mixture of simi
lar to 44% EETA79001 lithology B (ferroan basalt) and similar to 56% of All
an Hills A77005 (ALHA7705) light lithology (incompatible element-poor Iherz
olite). Micro-instrumental neutron activation analysis ((INAA) data on xeno
cryst-free groundmass samples of lithology A show that about 20-25% of the
melt phase could be dissolved Iherzolite. The bulk and groundmass samples o
f lithology A have excesses in Au, which indicates either meteoritic contam
ination or addition by some unknown martian geochemical process.
Previous workers have suggested that lithology A was formed by either assim
ilation of cumulates (like ALHA77005), by a basalt (like lithology B), or b
y mixing of basaltic and Iherzolitic magmas. The former scenario is energet
ically improbable and unlikely to explain the normal Fe/Mg zonation in lith
ology A groundmass pyroxenes, whereas the latter scenario is unlikely to sa
tisfy the constraints of the mixing model indicating the ultramafic compone
nt is poor in incompatible elements. We suggest rather that EETA79001 litho
logy A is an impact melt composed dominantly of basalt like lithology B and
Iherzolitic cumulates like the trace-element-poor fraction of ALHA77005 or
Y-793605. This model can satisfy the energetic, petrologic, and geochemica
l constraints imposed by the samples. If EETA79001 lithology A is an impact
melt, this would have considerable consequences for current models of mart
ian petrologic evolution. It would call into question the generally accepte
d age of magmatism of martian basalts and preclude the use of lithology A g
roundmass as a primary martian basalt composition in experimental studies.
Regardless, the latter is required because lithology A groundmass is a hybr
id composition.