|— Group —|
|Weston meteorite, H4|
|Parent body||Possibly 6 Hebe, less likely 3 Juno & 7 Iris|
|Composition||Iron ~25-31%, bronzite (an orthopyroxene), olivine (with characteristic fayalite (Fa) content 16 to 20 mol%), nickel-iron 15-19%, troilite 5%|
|Petrologic type||3 (~2.5%), 5 (40%), 4 & 6 (57.5%)|
|Alternative names||Bronzite chondrites, Olivine bronzite chondrites|
|Nuevo Mercurio, H5|
The name comes from their High iron abundance, with respect to other ordinary chondrites.
Historically, the H chondrites have been named bronzite chondrites or olivine bronzite chondrites for the dominant minerals, but these terms are now obsolete.
Parent body 
A probable parent body for this group is the S-type asteroid 6 Hebe, with less likely candidates being 3 Juno and 7 Iris. It is supposed that these meteorites arise from impacts onto small near-earth asteroids broken off from 6 Hebe in the past, rather than originating from 6 Hebe directly.
Their high iron abundance is about 25-31% by weight. Over half of this is present in metallic form, making these meteorites strongly magnetic despite the stony chondritic appearance.
The most abundant minerals are bronzite (an orthopyroxene), and olivine. Characteristic is the fayalite (Fa) content of the olivine of 16 to 20 mol%. They contain also 15-19% of nickel-iron metal and about 5% of troilite. The majority of these meteorites have been significantly metamorphosed, with over 40% being in petrologic class 5, most of the rest in classes 4 and 6. Only a few (about 2.5%) are of the largely unaltered petrologic class 3.
See also