Abstract
Shergottite is the largest group of Martian meteorites.
In this study, we investigated the formation sequence and relationship of enriched shergottites with MELTS calculation by using their estimated melt compositions.
We used nine enriched shergottites for sample and these four samples are non-cumulate rocks.We employed bulk composition of two non-cumulate Olivine-Phyric samples as the starting melt composition of enriched shergottites.
The results of MELTS calculation suggested that a similar composition to the bulk compositions of Los Angeles and Dhofar 378 (Basaltic and non-cumulate samples) could be produced at 1110 and 1040 degrees Celsius.
This study demonstrates that these nine enriched shergottites may have been formed by the same magmatic event as they show similar crystallization and exposure ages.
