Schematic example illustration for the knowledge article “Martian meteorites”
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Detailed explanation

Chemistry, isotopes, ages and gases trapped in some samples connect these meteorites to Mars.

Principal groups are shergottites, nakhlites and chassignites, with rare orthopyroxenites and basaltic breccias.

Main groups
shergottite · nakhlite · chassignite

Placed in context

Groups and subgroups

These cards show the next classification level. Linked groups open their own detailed explanation.

Shergottites

The largest Martian-meteorite group; basaltic, olivine-rich or lherzolitic igneous rocks.

Nakhlites

Clinopyroxene-rich cumulate Martian rocks that can contain evidence of later aqueous alteration.

Chassignites

Rare olivine-rich Martian meteorites of dunitic composition.

Orthopyroxenite

The ALH 84001 type consists mainly of orthopyroxene and sits outside the three classic SNC groups.

Regolith breccia

NWA 7034 and paired finds contain diverse Martian crust fragments in a polymict breccia.

How material leaves Mars

Only highly energetic impacts can accelerate near-surface rock without completely destroying it. Travel times and terrestrial find histories differ from specimen to specimen.

Evidence for a Martian origin

The strongest evidence comes from gases trapped in shock-melted inclusions whose composition matches the Martian atmosphere measured by spacecraft. Oxygen isotopes, mineral chemistry and comparatively young crystallisation ages reinforce the case.

Attribution is therefore not based on red colour. Many Martian meteorites look grey, greenish or black, while terrestrial basalts may appear similar. Laboratory evidence is required.

Major groups and their rocks

Shergottites are the most common group and range from basaltic to olivine-rich rocks. Nakhlites are clinopyroxene-rich cumulates, chassignites olivine-rich intrusive rocks. The orthopyroxenite ALH 84001 records a much older history.

Regolith breccias can mix Martian surface material and atmospheric components. All were launched by very large impacts; the challenge is achieving escape speed without melting all ejected rock.

Short & simple

The essentials in 30 seconds

  • Igneous rocks from Mars launched into space by large impacts.
  • Chemistry, isotopes, ages and gases trapped in some samples connect these meteorites to Mars.
  • Principal groups are shergottites, nakhlites and chassignites, with rare orthopyroxenites and basaltic breccias.

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Sources & databases

Editorially paraphrased and expanded from the linked specialist and primary sources; reviewed 24 August 2026. New classifications and database entries may require later updates.