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Martian meteorite (SNC meteorites)
— Clan —
Martian meteorite EETA79001, shergottite
TypeAchondrite
Subgroups
Parent bodyMars
Total known specimens277 as of 15 September 2020[1]
Martian meteorite NWA 7034, nicknamed "Black Beauty," weighs approximately 320 g (11 oz).[2]

A Martian meteorite is a rock that formed on Mars, was ejected from the planet by an impact event, and traversed interplanetary space before landing on Earth as a meteorite. As of September 2020, 277 meteorites had been classified as Martian, less than half a percent of the 72,000 meteorites that have been classified.[1] The second largest complete, uncut Martian meteorite, Taoudenni 002,[3] was recovered in Mali in early 2021. It weighs 14.5 kilograms (32 pounds) and is on display at the Maine Mineral and Gem Museum.

There are three groups of Martian meteorite: shergottites, nakhlites and chassignites, collectively known as SNC meteorites. Several other Martian meteorites are ungrouped. These meteorites are interpreted as Martian because they have elemental and isotopic compositions that are similar to rocks and atmospheric gases on Mars, which have been measured by orbiting spacecraft, surface landers and rovers.[4][5] The term does not include meteorites found on Mars, such as Heat Shield Rock.

History

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By the early 1980s, it was obvious that the SNC group of meteorites (Shergottites, Nakhlites, and Chassignites) were significantly different from most other meteorite types. Among these differences were younger formation ages, a different oxygen isotopic composition, the presence of aqueous weathering products, and some similarity in chemical composition to analyses of the Martian surface rocks in 1976 by the Viking landers. Several scientists suggested these characteristics implied the origin of SNC meteorites from a relatively large parent body, possibly Mars.[6][7]

Then in 1983, various trapped gases were reported in impact-formed glass of the EET79001 shergottite, gases which closely resembled those in the Martian atmosphere as analyzed by Viking.[8] These trapped gases provided direct evidence for a Martian origin. In 2000, an article by Treiman, Gleason, and Bogard gave a survey of all the arguments used to conclude that the SNC meteorites (of which 14 had been found at the time) were from Mars. They wrote, "There seems little likelihood that the SNCs are not from Mars. If they were from another planetary body, it would have to be substantially identical to Mars as it now is understood."[4]

Subdivision

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The Martian meteorites are divided into three groups (orange) and two grouplets (yellow). SHE = Shergottite, NAK = Nakhlite, CHA = Chassignite, OPX = Orthopyroxenite (ALH 84001), BBR = Basaltic Breccia (NWA 7034).

As of April 25, 2018, 192 of the 207 Martian meteorites are divided into three rare groups of achondritic (stony) meteorites: shergottites (169), nakhlites (20), chassignites (3), and ones otherwise (15) (containing the orthopyroxenite (OPX) Allan Hills 84001, as well as 10 basaltic breccia meteorites).[1] Consequently, Martian meteorites as a whole are sometimes referred to as the SNC group (pronounced /snɪk/).[9] They have isotope ratios that are consistent with each other and inconsistent with a terrestrial origin. The names derive from the location of where the first meteorite of their type was discovered.

Shergottites

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Roughly three-quarters of all Martian meteorites can be classified as shergottites. They are named after the Shergotty meteorite, which fell at Sherghati, India in 1865.[10] Shergottites are igneous rocks of mafic to ultramafic lithology. They fall into three main groups, the basaltic, olivine-phyric (such as the Tissint group found in Morocco in 2011[11][12]) and lherzolitic shergottites, based on their crystal size and mineral content. They can be categorised alternatively into three or four groups based on their rare-earth element content.[13] These two classification systems do not line up with each other, hinting at complex relationships between the various source rocks and magmas from which the shergottites formed.

NWA 6963,[14] a shergottite found in Morocco, September 2011.

The shergottites appear to have crystallised as recently as 180 million years ago,[15] which is a surprisingly young age considering how ancient the majority of the surface of Mars appears to be, and the small size of Mars itself. Because of this, some have advocated the idea that the shergottites are much older than this.[16] This "Shergottite Age Paradox" remains unsolved and is still an area of active research and debate.

It has been suggested the 3-million-year-old crater Mojave, 58.5 km in diameter, was a potential source of these meteorites.[17] A paper published in 2021, however, disputes this, proposing instead the 28 km crater Tooting, or possibly the crater 09-000015 as the crater source of the depleted olivine-phyric shergottites ejected 1.1 Ma ago.[18][19]

Nakhlites

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Nakhla meteorite's two sides and its inner surfaces after breaking it
Main article: Nakhlite

Nakhlites are named after the first of them, the Nakhla meteorite, which fell in El-Nakhla, Alexandria, Egypt in 1911 and had an estimated weight of 10 kg.

Nakhlites are igneous rocks that are rich in augite and were formed from basaltic magma from at least four eruptions, spanning around 90 million years, from 1416 ± 7 to 1322 ± 10 million years ago.[20] They contain augite and olivine crystals. Their crystallization ages, compared to a crater count chronology of different regions on Mars, suggest the nakhlites formed on the large volcanic construct of either Tharsis, Elysium, or Syrtis Major Planum.[21]

It has been shown that the nakhlites were suffused with liquid water around 620 million years ago and that they were ejected from Mars around 10.75 million years ago by an asteroid impact. They fell to Earth within the last 10,000 years.[21]

Chassignites

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The first chassignite, the Chassigny meteorite, fell at Chassigny, Haute-Marne, France in 1815. There has been only one other chassignite recovered, named Northwest Africa (NWA) 2737. NWA 2737 was found in Morocco or Western Sahara in August 2000 by meteorite hunters Bruno Fectay and Carine Bidaut, who gave it the temporary name "Diderot." It was shown by Beck et al.[22] that its "mineralogy, major and trace element chemistry as well as oxygen isotopes revealed an unambiguous Martian origin and strong affinities with Chassigny."

Ungrouped meteorites

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Allan Hills 84001 (ALH 84001)

Among these, the famous specimen Allan Hills 84001 has a different rock type from other Martian meteorites: it is an orthopyroxenite (an igneous rock dominantly composed of orthopyroxene). For this reason, it is classified within its group, the "OPX Martian meteorites". This meteorite received much attention after an electron microscope revealed structures that were considered to be the fossilized remains of bacteria-like lifeforms. As of 2005, scientific consensus was that the microfossils were not indicative of Martian life, but of contamination by earthly biofilms. ALH 84001 is as old as the basaltic and intermediate shergottite groups – i.e., 4.1 billion years old.[citation needed]

In March 2004 it was suggested that the unique Kaidun meteorite, which landed in Yemen on December 3, 1980,[23] may have originated on the Martian moon of Phobos.[24] Because Phobos has similarities to C-type asteroids and because the Kaidun meteorite is a carbonaceous chondrite, Kaidun is not a Martian meteorite in the strict sense. However, it may contain small fragments of material from the Martian surface.

The Martian meteorite NWA 7034 (nicknamed "Black Beauty"), found in the Sahara desert during 2011, has ten times the water content of other Mars meteorites found on Earth.[2] The meteorite contains components as old as 4.42 ± 0.07 Ga (billion years),[25] and was heated during the Amazonian geologic period on Mars.[26]

A meteorite that fell in 1986 in Dayanpo, China, contained a magnesium silicate mineral called "Elgoresyte", a mineral not found on Earth.[27]

Origin

[edit]

The majority of SNC meteorites are quite young compared to most other meteorites and seem to imply that volcanic activity was present on Mars only a few hundred million years ago. The young formation ages of Martian meteorites was one of the early recognized characteristics that suggested their origin from a planetary body such as Mars. Among Martian meteorites, only ALH 84001 and NWA 7034 have radiometric ages older than about 1400 Ma (Ma = million years). All nakhlites, as well as Chassigny and NWA 2737, give similar if not identical formation ages around 1300 Ma, as determined by various radiometric dating techniques.[15][28] Formation ages determined for many shergottites are variable and much younger, mostly ~150–575 Ma.[15][29][30][31]

The chronological history of shergottites is not totally understood, and a few scientists have suggested that some may have formed prior to the times given by their radiometric ages,[32] a suggestion not accepted by most scientists. Formation ages of SNC meteorites are often linked to their cosmic-ray exposure (CRE) ages, as measured from the nuclear products of interactions of the meteorite in space with energetic cosmic ray particles. Thus, all measured nakhlites give essentially identical CRE ages of approximately 11 Ma, which, when combined with their possible identical formation ages, indicates ejection of nakhlites into space from a single location on Mars by a single impact event.[15] Some of the shergottites also seem to form distinct groups according to their CRE ages and formation ages, again indicating ejection of several different shergottites from Mars by a single impact. However, CRE ages of shergottites vary considerably (~0.5–19 Ma),[15] and several impact events are required to eject all the known shergottites. It had been asserted that there are no large young craters on Mars that are candidates as sources for the Martian meteorites, but subsequent studies claimed to have a likely source for ALH 84001,[33] and a possible source for other shergottites.[34]

In a 2014 paper, several researchers claimed that all Shergottite meteorites come from the Mojave Crater on Mars.[17]

Age estimates based on cosmic ray exposure

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A Martian meteorite crafted into a small pendant and suspended from a silver necklace.

The amount of time spent in transit from Mars to Earth can be estimated by measurements of the effect of cosmic radiation on the meteorites, particularly on isotope ratios of noble gases. The meteorites cluster in families that seem to correspond to distinct impact events on Mars. It is thought that the meteorites all originate in relatively few impacts every few million years on Mars. The impactors would be kilometers in diameter, and the craters they form on Mars would be tens of kilometers in diameter. Models of impacts on Mars are consistent with these findings.[35]

Ages since impact determined so far include[36][37]

Type Age (mya)
Dhofar 019, olivine-phyric shergottite 19.8 ± 2.3[35]
ALH 84001, orthopyroxenite 15.0 ± 0.8[35]
Dunite (Chassigny) 11.1 ± 1.6[35]
Six nakhlites 10.8 ± 0.8[20][35]
Lherzolites 3.8–4.7[35]
Six basaltic shergottites 2.4–3.0[35]
Five olivine-phyric shergottites 1.2 ± 0.1[35]
EET 79001 0.73 ± 0.15[35]

Possible evidence of life

[edit]

Several Martian meteorites have been found to contain what some think is evidence for fossilized Martian life forms. The most significant of these is a meteorite found in the Allan Hills of Antarctica (ALH 84001). Ejection from Mars seems to have taken place about 16 million years ago. Arrival on Earth was about 13,000 years ago. Cracks in the rock appear to have filled with carbonate materials (implying groundwater was present) between 4 and 3.6 billion years ago. Evidence of polycyclic aromatic hydrocarbons (PAHs) have been identified with the levels increasing away from the surface. Other Antarctic meteorites do not contain PAHs. Earthly contamination should presumably be highest at the surface. Several minerals in the crack fill are deposited in phases, specifically, iron deposited as magnetite, which are claimed to be typical of biodepositation on Earth. There are also small ovoid and tubular structures that might be nanobacteria fossils in carbonate material in crack fills (investigators McKay, Gibson, Thomas-Keprta, Zare).[38] Micropaleontologist Schopf, who described several important terrestrial bacterial assemblages, examined ALH 84001 and opined that the structures are too small to be Earthly bacteria and don't look especially like lifeforms to him. The size of the objects is consistent with Earthly "nanobacteria", but the existence of nanobacteria itself has been largely discredited.[39][40]

Many studies disputed the validity of the fossils.[41][42] For example, it was found that most of the organic matter in the meteorite was of terrestrial origin.[43] But, a 2009 study suggests that magnetite in the meteorite could have been produced by Martian microbes. The study, published in the Journal of the Geochemical and Meteoritic Society, used more advanced high-resolution electron microscopy than was possible in 1996.[44] A serious difficulty with the claims for a biogenic origin of the magnetites is that the majority of them exhibit topotactic crystallographic relationships with the host carbonates (i.e., there are 3D orientation relationships between the magnetite and carbonate lattices), which is strongly indicative that the magnetites have grown in-situ by a physico-chemical mechanism.[45]

While water is no indication of life, many of the meteorites found on Earth have shown water, including NWA 7034 which formed during the Amazonian period of Martian geological history.[46] Other signs of surface liquid water on Mars (such as recurring slope lineae[47]) are a topic of debate among planetary scientists, but generally consistent with the earlier evidence provided by Martian meteorites. Any liquid water present is likely too minimal to support life.

See also

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References

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Revisions and contributorsEdit on WikipediaRead on Wikipedia

Martian meteorite

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Martian meteorites are fragments of rock ejected from the surface of Mars by or impacts, which then travel through space and land on after surviving . They are classified as achondritic meteorites, primarily igneous in origin, and represent the only direct physical samples of Mars available for laboratory analysis prior to planned sample-return missions. As of 2025, approximately 400 individual Martian meteorites have been officially recognized by the Meteoritical Society, with a combined mass of approximately 374 kg, though many are fragments from fewer distinct ejection events. These meteorites are identified as Martian through multiple lines of evidence, most conclusively the composition of trapped in impact-produced melt glass inclusions, which matches the isotopic ratios measured in the Martian atmosphere by Viking landers and subsequent orbiters. Additional confirmation comes from their oxygen ratios, which plot on a distinct line separate from or lunar materials, and their mineralogies consistent with under Mars' higher pressure and oxidizing conditions. The meteorites' young ages—ranging from about 150 million to 1.3 billion years for most—indicate derivation from relatively recent volcanic activity compared to ancient lunar samples. The primary classification groups Martian meteorites into the SNC suite—named for the falls of Shergotty (India, 1865), Nakhla (Egypt, 1911), and Chassigny (France, 1815)—which encompasses over 90% of known specimens. Shergottites, the most abundant subgroup, are basaltic to lherzolitic rocks formed from mantle-derived magmas; nakhlites are clinopyroxene-rich cumulates; and chassignites are olivine-rich dunites. Distinct outliers include the orthopyroxenite ALH 84001, recovered from Antarctica and dated to about 4.1 billion years old, and the polymict breccia NWA 7034 (paired with NWA 7533), which contains ancient zircons up to 4.5 billion years old and evidence of prolonged aqueous alteration. Analysis of Martian meteorites has profoundly advanced understanding of the planet's , revealing a basaltic crust with evidence of past water-rock interactions through hydrated silicates, , and sulfates. For instance, ALH 84001 preserves globules formed in a potentially habitable subsurface environment around 3.9 billion years ago, while NWA 7034 indicates multiple episodes of spanning Mars' history. These samples also calibrate spectroscopic data from Mars missions, constrain mantle composition and evolution, and inform by providing clues to ancient environmental conditions suitable for life.

Overview

Definition

Martian meteorites are fragments of rock ejected from the surface or interior of Mars by impacts with asteroids or comets, which accelerate material into interplanetary space; these fragments then intersect and survive to land as meteorites. They primarily represent samples of the Martian crust and mantle, providing of Mars' geological . Unlike the vast majority of meteorites, which originate from asteroids, Martian meteorites are achondrites—differentiated rocks lacking chondrules—and are distinguished by their chemical and isotopic signatures matching those observed in Martian meteorites by orbiters and landers. The primary classification of Martian meteorites encompasses the SNC group, named after the three initial subgroups: shergottites (basaltic to lherzolitic rocks), nakhlites (augite-rich clinopyroxenites), and chassignites (olivine-rich dunites), all of which formed as igneous rocks through and during Mars' volcanic history or in its early epoch. In addition to the SNC meteorites, several ungrouped specimens, such as the orthopyroxenite ALH 84001, expand the known diversity, though they share the overarching Martian affinity. These rocks crystallized from mantle-derived magmas between approximately 150 million and 4.5 billion years ago, reflecting episodes of intense and impact processing on Mars. As of November 2025, 401 Martian meteorites have been officially recognized by the Meteoritical Society, with a total known mass of approximately 374 kilograms, predominantly recovered from hot and cold deserts like and . Notable recent finds include NWA 16788, the largest known individual Martian meteorite at 24.67 kg, classified in 2025. This collection represents less than 0.6%—of the over 78,000 known meteorites on , underscoring their rarity compared to other planetary-sourced materials, such as the approximately 785 lunar meteorites or the more than 1,000 howardite-eucrite-diogenite (HED) meteorites believed to originate from the Vesta. The limited abundance highlights the infrequent ejection events and survival trajectories required for interplanetary transfer from Mars.

Identification

The identification of meteorites as originating from Mars relies on multiple lines of geochemical evidence that distinguish them from terrestrial rocks or meteorites from other bodies. The process began in the early 1980s when analyses of trapped gases in the meteorite Elephant Moraine 79001 (EET 79001) revealed noble gas compositions matching those measured in the Martian atmosphere by the Viking landers in 1976, particularly the elevated 40^{40}Ar/36^{36}Ar ratio of approximately 3000—far higher than Earth's value of about 300—indicating entrapment of Martian atmospheric gases during shock-induced melting on Mars. This discovery provided the first definitive link between the Shergottite-Nakhlite-Chassignite (SNC) group of achondritic meteorites and Mars, as the gas signatures could not be explained by terrestrial contamination or implantation. Further confirmation comes from the isotopic composition of trapped and other elements, including nitrogen-15 enrichment with δ15^{15}N values around +620‰—much heavier than Earth's atmospheric —and isotope ratios such as 129^{129}Xe/132^{132}Xe ≈ 2.40, both consistent with Viking measurements of the Martian atmosphere and indicative of processes on Mars. Oxygen isotope ratios in Martian meteorites, expressed as δ17^{17}O and δ18^{18}O relative to the , plot along a distinct Martian Line (MFL) with a of approximately 0.53 and an offset Δ17^{17}O of 0.32‰, separate from the Terrestrial Fractionation Line (TFL) and those of lunar or asteroidal materials. This fractionation arises from Mars' unique mantle and atmospheric processing, providing robust evidence against an Earth-based origin. To exclude terrestrial alteration, scientists examine weathering products and the fusion crust—the thin, glassy outer layer formed during . Fusion crusts on suspected Martian meteorites typically show minimal post-arrival , with internal secondary minerals like carbonates or iddingsite limited to pre-terrestrial Martian aqueous processes, as confirmed by spectroscopic and petrographic that distinguishes them from widespread terrestrial oxidation. These combined methods ensure that only meteorites exhibiting all key Martian signatures are classified as such, with ongoing refinements from missions like validating the trapped gas and criteria.

History

Early Discoveries

The earliest documented discovery of what would later be recognized as a Martian meteorite occurred on October 3, 1815, when the Chassigny meteorite fell in Chassigny, , producing a loud report heard across the region. Weighing approximately 4 kilograms upon recovery, fragments were collected shortly after the event and described in contemporary accounts as a greenish, crystalline stone resembling olivine-rich rock. Initially classified as a rare due to its lack of chondrules and igneous texture, Chassigny was housed in European museums as an unusual basaltic specimen without any suspected extraterrestrial planetary origin beyond or asteroids. Subsequent finds reinforced this pattern of classification. On August 25, 1865, the Shergotty meteorite, a 5-kilogram stone, fell in , , , after witnesses observed a bright fireball and detonations; it was quickly recovered and noted for its dark, glassy fusion crust and basaltic composition. Like Chassigny, Shergotty was categorized as an and preserved in collections such as the in Calcutta, valued for its fine-grained texture but interpreted solely as a differentiated meteorite from the . By the early , the Nakhla meteorite added to this trio when it fell on June 28, 1911, near Alexandria, Egypt, showering approximately 40 stones totaling 10 kilograms over several kilometers; eyewitnesses reported the fragments as hot and fresh, with minimal weathering observed in initial examinations. Nakhla's dark, pyroxene-rich matrix led to its prompt identification as another , with samples distributed to institutions like the , where it was studied as a cumulate . Prior to the 1970s, these SNC meteorites—named for Shergotty, Nakhla, and Chassigny—represented just a handful among over 100 known achondrites collected worldwide, all grouped under terrestrial-like igneous rocks without links to a specific planetary body. Early analyses relied on basic petrographic microscopy and , which revealed their mineralogy but lacked the precision for or isotopic distinctions that might have hinted at unique origins. Limited instrumentation, such as rudimentary spectrometers, hindered detection of subtle volatile contents or atmospheric trapped gases, leaving these meteorites as enigmatic rarities in museum vaults rather than keys to .

Recognition as Martian

The recognition of certain achondritic meteorites as originating from Mars began with the establishment of a compositional baseline for the planet's atmosphere during the Viking missions. In 1976, the Viking landers' Gas Chromatograph Mass Spectrometer (GCMS) instruments measured the noble gas abundances in Mars' atmosphere, revealing enrichments in argon (about 1.6% by volume), krypton, and xenon relative to Earth, along with specific isotopic ratios such as elevated ¹³⁶Xe/¹³²Xe. These measurements provided the first direct reference for comparing potential Martian samples, enabling later noble gas analyses to test extraterrestrial origins. A breakthrough came in 1983 with the analysis of the Antarctic shergottite Elephant Moraine A79001 (EETA 79001), recovered in 1979. Researchers Donald D. Bogard and Pratt Johnson identified trapped noble gases in shock-produced melt glass pockets within the meteorite, exhibiting elemental abundances and isotopic compositions—such as ⁸⁴Kr/¹³²Xe ratios of approximately 20 and ¹²⁹Xe/¹³²Xe of about 2.5—that closely matched the Viking atmospheric data. This suggested that the gases were shock-implanted from Mars' atmosphere during ejection by impact, marking the first strong evidence linking a meteorite to the Red Planet. Building on this, a 1984 study by Robert H. Becker and Robert O. Pepin further corroborated the Martian origin by examining nitrogen and noble gas systematics in EETA 79001, demonstrating that the trapped volatiles aligned with Mars' thin, CO₂-dominated atmosphere rather than terrestrial or other solar system sources. The Antarctic Search for Meteorites (ANSMET) program, initiated by the U.S. in 1976, played a crucial role in expanding the sample set available for study. Expeditions in the late and recovered key specimens like 77005 (1977), the first shergottite identified by ANSMET, and others that bolstered comparative analyses. By the 1990s, accumulating evidence from oxygen compositions—where SNC meteorites (shergottites, nakhlites, and chassignites) define a distinct fractionation line with Δ¹⁷O ≈ +0.32‰, separate from Earth's—combined with mineralogical similarities to Martian surface compositions observed by orbiters, led to on their Martian . This validation transformed the SNC group into a cornerstone for understanding Mars' geology.

Modern Collections and Recent Finds

The expansion of Martian meteorite collections since the has been driven by systematic searches in ice fields and hot desert regions, where natural processes concentrate meteorites for easier recovery. In , meteorite accumulation zones form where ice flows converge and surface melting exposes embedded rocks, a phenomenon exploited by programs like the U.S. Search for Meteorites (ANSMET) and Japan's Expedition. These efforts led to the discovery of ALH 84001 in the region on December 27, 1984, by ANSMET researchers, though its Martian origin was confirmed later; the , weighing 1.93 kg, provided key insights into ancient Martian crust. Similarly, Yamato 000593, a 13.7 kg nakhlite, was recovered from the Yamato in 2000 by the Japanese expedition, highlighting the role of such zones in yielding large, well-preserved specimens. Hot desert regions, particularly Northwest Africa (NWA), have contributed the majority of post-1990s finds due to wind erosion that strips away soil cover and exposes dark fusion-crusted rocks against light sands. Since the late 1990s, private and institutional hunters have recovered over 149 NWA-classified Martian meteorites, representing a surge from fewer than a dozen prior to that era. These samples, often shergottites or breccias, have diversified collections by including rarer types like the basaltic NWA 7034 (""), found in 2011 in the Moroccan . By 2025, approximately 400 individual Martian meteorites are recognized, with about 70% originating from hot deserts such as those in Northwest Africa, , and the , compared to roughly 20-30 from sites. Among recent highlights is NWA 16788, the largest known individual Martian specimen at 25 kg, discovered by a hunter in 's on November 16, 2023; classified as a shergottite, it was auctioned at in New York on July 16, 2025, for $5.3 million. In 2025, launched an investigation into the legality of NWA 16788's export, citing concerns over illicit trafficking and suspending meteorite and precious stone exports pending review. Concurrently, Yamato 000593 was displayed at the Japan Pavilion during in , allowing public interaction with a while the original underscored Japan's contributions to Martian sample recovery.

Classification

Shergottites

Shergottites comprise the largest and most diverse group of Martian meteorites, accounting for approximately 85% of the known collection by number and 90% by mass as of November 2025. Named after the Shergotty meteorite, which fell in Shergotty, India, on August 25, 1865, this subgroup is characterized by its basaltic to ultramafic compositions derived from Martian mantle sources. These meteorites exhibit a range of textural varieties, reflecting diverse crystallization conditions in Martian volcanic environments. Shergottites are petrographically subdivided into basaltic, olivine-phyric, lherzolitic, and poikilitic subtypes, with some classified as gabbroic variants. Their crystallization ages, determined through methods such as Rb-Sr, Sm-Nd, and U-Pb, span approximately 150 to 600 million years, indicating relatively recent volcanic activity on Mars during the Amazonian period. This age range highlights the dynamic nature of Martian , with enriched and depleted geochemical signatures suggesting differentiation within the planet's mantle. The primary minerals in shergottites include pyroxenes such as pigeonite and , , and maskelynite, which is a diaplectic formed from shocked . These assemblages reflect fractional crystallization of magmas, with pyroxenes often showing zoning that records cooling histories. Shock features, including maskelynite and melt pockets, are ubiquitous, resulting from high-pressure impacts on Mars that facilitated ejection to . Notable examples include the Zagami meteorite, a witnessed fall in on October 3, 1962, representing a fine-grained basaltic shergottite with rapid cooling textures. Another key specimen is Northwest Africa (NWA) 16788, recovered in 2023 and recognized as the largest known individual Martian meteorite at approximately 24.7 kilograms, classified as an enriched microgabbroic shergottite. These samples provide critical insights into the compositional variability and impact histories of shergottites, underscoring their role as proxies for Martian mantle-derived .

Nakhlites

Nakhlites form a clinopyroxene-rich subgroup of Martian meteorites, representing cumulate igneous rocks derived from basaltic magmas during prolonged . Approximately 33 specimens are known as of November 2025, including both observed falls and finds. The group is named after the Nakhla meteorite, an 10 kg stone that fell on June 28, 1911, near Nakhla Falls in Egypt's . These meteorites are petrologically uniform, suggesting origin from a common parental in shallow intrusions or lava flows, likely associated with the volcanic province. The primary mineral in nakhlites is , forming large cumulate crystals with cores enriched in magnesium (Mg# ≈ 63) and rims more iron-rich. Interstitial phases include (bytownite), (Mg# ≈ 42 in cores, more fayalitic in rims), and a fine-grained mesostasis composed of , alkali , and opaque oxides like titanomagnetite. Post-magmatic alteration has produced iddingsite, a hydrous assemblage of clays, iron oxyhydroxides, , and carbonates, which rims grains and indicates interaction with aqueous fluids at low temperatures. Some specimens, such as MIL 03346, contain a distinctive black y matrix within the mesostasis, reflecting rapid cooling. Trace minerals include , sulfides (), and halides. The age of nakhlites is uniformly about 1.3 billion years, determined from Rb-Sr, Sm-Nd, and Pb-Pb isotope systematics, while cosmic-ray exposure ages cluster around 10-15 million years, consistent with a single ejection event from Mars. Prominent examples include the Lafayette meteorite, a 0.8 kg stone found in 1931 in Purdue Farm, , , notable for its well-preserved iddingsite veins; Governador Valadares, a 1.4 kg find from 1958 in , , with coarse phenocrysts; and the Nakhla type specimen itself. Other significant members are the paired finds Yamato 000593 and Northwest Africa 998, which exhibit minimal terrestrial . These samples highlight the nakhlites' role in elucidating Martian mantle processes, aqueous alteration, and the longevity of volcanic activity on the planet.

Chassignites

Chassignites form a rare subgroup of Martian meteorites, with only three officially recognized specimens: the historical Chassigny fall from 1815 in , Northwest Africa (NWA) 2737 discovered in 2000, and NWA 8694 found in 2015. These ultramafic rocks are distinguished by their , representing less than 1% of all known Martian meteorites and providing unique samples of deep-seated magmatic processes on Mars. The composition of chassignites is dominated by over 90% , primarily magnesium-rich (Fo 75–92), accompanied by subordinate amounts of orthopyroxene, clinopyroxene, , and . They exhibit a coarse-grained cumulate texture, featuring large (up to several millimeters), anhedral to subhedral olivine crystals with interstitial pyroxenes and minor phases, indicative of gravitational settling in a slowly cooling . This texture, preserved with relatively low shock levels (typically <30 GPa), contrasts with the more fragmented or shocked states of many other SNC meteorites. Chassignites crystallized approximately 1.1–1.4 billion years ago, based on Rb-Sr, Sm-Nd, and other radiometric dating, marking them as among the older igneous rocks in the Martian meteorite collection. A prominent example is NWA 2737, a 611-gram stone paired with related finds like NWA 1950, whose olivine-hosted melt inclusions reveal a parental magma composition consistent with primitive, high-temperature melts akin to , with elevated magnesium and low incompatible elements. These meteorites are interpreted as cumulates from the Martian mantle, offering direct evidence of primitive, undepleted material from depths of 50–200 km, and thus key insights into the planet's early differentiation and volatile inventory.

Ungrouped Meteorites

Ungrouped Martian meteorites comprise a small but significant portion of the known collection, representing less than 12% of over 400 classified samples as of November 2025, and are distinguished by their failure to align with the primary SNC groups despite confirmation of Martian origin through trapped noble gases and oxygen isotopic ratios matching the Martian atmosphere. These meteorites often exhibit distinct petrologic and geochemical traits, such as older crystallization ages and complex histories involving impact melting or brecciation, providing evidence of diverse crustal processes not captured by the younger, igneous-dominated SNC meteorites. Recent classifications continue to add to this group, enhancing our understanding of Martian diversity. A prominent example is Allan Hills (ALH) 84001, an orthopyroxenite discovered in Antarctica in 1984, which crystallized approximately 4.1 billion years ago, making it one of the oldest known Martian samples. This meteorite consists primarily of low-calcium pyroxene with secondary carbonate globules, reflecting a history of shock metamorphism, thermal alteration, and possible aqueous interaction on Mars. ALH 84001 gained attention for controversial claims of biogenic features, such as magnetite chains within carbonates, though these remain debated and are further explored in studies of potential life evidence. Another key ungrouped specimen is Northwest Africa (NWA) 7034, nicknamed "Black Beauty," a polymict regolith breccia recovered from Morocco in 2011, containing zircon-bearing clasts with ages up to 4.5 billion years and a brecciation event around 2.1 billion years ago. Its composition includes mafic igneous fragments, impact-melted materials, and evidence of hydrothermal alteration, with bulk water content higher than typical SNC meteorites, indicating derivation from an ancient, water-altered Martian regolith. Over 50 paired stones, such as NWA 7533, expand this group, highlighting its representativeness of early Martian surface processes. The 2011 witnessed fall of Tissint, an olivine-phyric basaltic meteorite from Morocco, represents a transitional case with affinities to shergottites but distinct trace element patterns and shock features, including high-pressure minerals like ringwoodite, suggesting origins from a unique impact event on Mars. Recovered fresh, Tissint preserves organic compounds and atmospheric gases, underscoring the variability within ungrouped or atypical Martian materials. These ungrouped meteorites expand our sampling of the Martian crust, capturing ancient Noachian-era terrains through breccias and orthopyroxenites that reveal prolonged impact bombardment, hydrothermal activity, and geochemical diversity beyond the SNC suite. By including sedimentary and impact-derived components, they offer critical insights into Mars' early geological evolution and volatile history.

Physical and Chemical Properties

Mineralogy and Petrology

Martian meteorites are predominantly composed of basaltic and ultramafic rocks, with dominant silicate minerals including pyroxenes, olivines, and plagioclase (often shock-altered to maskelynite). Pyroxenes are the most abundant phase, typically pigeonite in shergottites and augite in nakhlites and chassignites, contrasting with the augite-dominated assemblages in many terrestrial basalts. Olivines are generally Mg-rich in shergottites, with core compositions ranging from Fo70 to Fo80, whereas in nakhlites they are more Fe-rich, with cores ranging from Fo40 to Fo45, indicating derivation from relatively primitive mantle sources. Maskelynite, a diaplectic glass formed by shock metamorphism of plagioclase (typically An50–60), is ubiquitous in shergottites and reflects impact pressures exceeding 30 GPa. Accessory minerals such as chromite, ilmenite, merrillite, and sulfides are common, comprising less than 5% of the modal mineralogy. Rock textures vary by subgroup, providing insights into crystallization histories. Shergottites exhibit porphyritic textures with olivine or pyroxene phenocrysts (up to 2.5 mm) set in a fine-grained groundmass of intergrown pyroxene and maskelynite, or coarser gabbroic and poikilitic varieties with oikocrystic pyroxenes enclosing chadacrysts. Nakhlites display cumulate textures dominated by equigranular augite (0.3–0.4 mm) and olivine, with interstitial plagioclase and mesostasis, suggesting slow cooling in shallow intrusions. Chassignites are dunites with coarse olivine cumulates (0.6 mm) and minor chromite, indicative of fractional crystallization in a magma chamber. Shock features, including melt pockets, veins, and fractured grains, are pervasive across all groups, while the outer fusion crust forms during atmospheric entry, typically 0.1–1 mm thick and enriched in volatiles. Petrogenesis of these meteorites involves crystallization from basaltic to picritic melts at low pressures (less than 0.1 GPa, corresponding to shallow crustal levels) and high temperatures around 1200°C, under relatively anhydrous conditions with water contents of 5–150 ppm. Zoning in pyroxenes and olivines reflects fractional crystallization sequences, starting with olivine and orthopyroxene on the liquidus, followed by pigeonite and augite. Evidence of aqueous alteration is prominent in nakhlites, where iddingsite—a mixture of phyllosilicates, magnetite, and carbonates—replaces olivine along fractures, pointing to post-magmatic hydrothermal activity at temperatures below 150°C. Mineral assemblages in Martian meteorites closely resemble those in basalts analyzed by rovers, such as the olivine-pyroxene-plagioclase assemblages in Gusev Crater rocks (Fo42–73) and Gale Crater sediments, confirming a shared basaltic crustal composition despite some variations in Fe/Mg ratios.

Geochemistry and Isotopes

Martian meteorites exhibit distinct major element compositions that reflect the geochemistry of their parent magmas and mantle sources. Compared to terrestrial basalts, they display higher FeO/MgO ratios, typically ranging from 0.5 to 1.0 in shergottites, indicating derivation from a more iron-rich mantle. Aluminum oxide (Al₂O₃) contents are notably lower, averaging 5-10 wt% in basaltic shergottites versus 14-18 wt% in Earth's mid-ocean ridge basalts, consistent with reduced plagioclase fractionation due to lower mantle pressures. Incompatible elements such as K, Ti, and P are enriched relative to refractory elements, pointing to metasomatized sources or partial melting under anhydrous conditions. Oxygen isotope systematics provide a key signature for distinguishing Martian meteorites from other achondrites. Their compositions plot along the Mars Fractionation Line (MFL) in δ¹⁷O versus δ¹⁸O space, with a slope of approximately 0.52 and an intercept of ~0.2‰, offset from the Terrestrial Fractionation Line by Δ¹⁷O ≈ 0.32‰. This mass-dependent fractionation reflects equilibrium processes in the Martian mantle and atmosphere, with bulk δ¹⁸O values typically 3.5-5.5‰ and δ¹⁷O 1.8-3.0‰ across subgroups like shergottites and nakhlites. Radiogenic isotope systems reveal significant heterogeneity in the Martian mantle. The Rb-Sr system yields initial ⁸⁷Sr/⁸⁶Sr ratios from 0.706 to 0.727, indicating variable Rb/Sr ratios and possible ancient crustal contamination in enriched samples. Sm-Nd analyses show εNd values ranging from +10 to +50 in depleted shergottites, reflecting long-term depletion in light rare earth elements (LREE) since early differentiation, while enriched varieties have negative εNd (-10 to -20), suggesting metasomatism or recycling. These variations, dated to 150-600 Ma crystallization ages, underscore a heterogeneous mantle with distinct reservoirs formed during the planet's accretion and magma ocean crystallization. Trace element patterns further illuminate mantle processes and core formation. Rare earth element (REE) profiles in enriched shergottites display LREE enrichment, with La/Yb ratios >10 and concave-upward shapes normalized to chondrites, contrasting with flatter patterns in depleted types. Siderophile elements like Ni, Co, and Ir are depleted by factors of 10-100 relative to chondrites, attributable to partitioning into a metallic core during early differentiation under reduced conditions (oxygen ~IW-1). Water contents in Martian meteorites indicate involvement of hydrous sources, with bulk H₂O up to 0.3 wt% in some nakhlites and chassignites, derived from primary amphiboles and apatites. Nominally minerals like and host 10-300 ppm H₂O, implying mantle source concentrations of 100-700 ppm, sufficient for minor hydrous melting without extensive alteration. These levels, combined with D/H ratios 2-7 times terrestrial, suggest primordial reservoirs modified by .

Origin and Journey to Earth

Ejection from Mars

Martian meteorites are ejected from the planet's surface primarily through impacts by asteroids or comets traveling at speeds exceeding 10 km/s. These collisions excavate typically 1–10 km in diameter and up to several kilometers deep, vaporizing a significant portion of the target material while accelerating fragments—thin slabs detached from the crater floor or walls—into space. The process relies on the mechanism, where reflected shock waves create tensile stresses that and propel material without excessive or fragmentation. Numerical simulations indicate that oblique impacts at angles of 30–45° are most efficient for producing intact capable of escape. The thin Martian crust, averaging approximately 50 km in thickness, facilitates ejection by allowing impacts to reach depths sufficient to access and launch underlying rock without requiring excessively large projectiles. Regions with locally thinner crust in the are considered potential source areas due to their geological history of intense bombardment and exposure of diverse lithologies matching meteorite compositions. During ejection, fragments must attain velocities greater than Mars' escape speed of 5 km/s to overcome the planet's and thin atmosphere. Models show that fragments from depths of up to 25–30 m can be launched with minimal deceleration, though only a tiny fraction survives intact: estimated survival rates of ejected mass reaching are less than 0.0001%, as most material either vaporizes, fragments, or falls back to Mars. High-velocity from the zone experience peak shock pressures of 20–45 GPa for durations of seconds, consistent with petrographic features like shock-induced melting and twinning observed in meteorites such as ALH 84001 and shergottites. These pressures align with hydrocode simulations of impacts producing craters 3–30 km wide. The frequency of successful ejections is low, with approximately 1 kg of Martian arriving on annually, based on collection rates and orbital dynamics models. Over Mars' 4-billion-year history, this implies a total ejected mass on the order of 10^{16} kg to account for known samples and losses during transit, highlighting the rarity of interplanetary transfer despite frequent impacts. Recent analyses suggest at least 10 discrete ejection events in the past 20 million years produced the bulk of recognized meteorites. Recent modeling (as of 2024) links many meteorites to ~10 young craters in the , with five craters sourcing about one-third of known SNC specimens.

Transit and Cosmic Ray Exposure

Martian meteorites ejected from the planet's surface undergo a prolonged interplanetary transit to , typically lasting 1 to 20 million years. This journey is governed by gravitational perturbations, particularly secular resonances in the inner solar system, which slowly evolve the orbits of the meter-sized fragments from Mars-crossing paths to Earth-intersecting ones. Dynamical simulations indicate that the minimum transit time is around 0.7 million years, with most deliveries occurring over 1 to 15 million years due to the efficiency of these resonant mechanisms in transporting without requiring close planetary encounters. During transit, the meteoroids are irradiated by galactic cosmic rays, high-energy particles that penetrate up to several meters into the material, producing cosmogenic nuclides such as ^{10}Be (half-life 1.387 Ma), ^{26}Al (0.717 Ma), and ^{36}Cl (0.301 Ma). These nuclides form primarily in the upper 1-2 meters of the meteoroid, where secondary particles from cosmic ray interactions dominate , allowing researchers to infer pre-atmospheric sizes and irradiation geometries. The resulting cosmogenic records provide key evidence of the meteoroids' exposure history, with production rates varying by depth and composition, as seen in analyses of shergottite and nakhlite samples. Cosmic ray exposure ages for shergottites exhibit a bimodal distribution, clustering around 3 Ma and approximately 20 Ma, reflecting multiple distinct ejection events from Mars and subsequent fragmentation in space. These ages, derived from and concentrations, correspond to shielding depths of 0.5-2 m in the parent bodies, indicating launch from sizable impact fragments rather than small debris. In contrast, nakhlites and chassignites share a more uniform exposure age of about 11 Ma, suggesting a single launch event. For instance, at least 17 Northwest Africa (NWA) nakhlite specimens, including NWA 998, NWA 817, and NWA 5790, form a paired group with indistinguishable exposure ages, confirming their origin from the same . Upon reaching , the meteoroids experience intense heating and during at velocities of 10-15 km/s, resulting in 50-90% mass loss through and of the outer layers. This forms a fusion crust typically 0.5-2 mm thick and reduces the original size significantly, with surviving fragments often representing only 10-50% of the pre-entry mass, as modeled for specimens like ALH 77005. The process ensures that only robust, meter-scale progenitors deliver recoverable meteorites to the surface.

Age Determination Methods

Age determination of Martian meteorites employs radiometric techniques to establish ages of the parent magmas, ejection ages from Mars due to impact events, and exposure ages during interplanetary transit. These methods rely on isotopic systems sensitive to different and conditions, providing a timeline from formation to arrival on . Crystallization ages reflect the igneous history, while ejection and exposure ages constrain the timing and duration of the meteorites' journey. Crystallization dating primarily uses long-lived isotopic systems unaffected by later impacts. For ancient meteorites like ALH 84001, classified as an orthopyroxenite, U-Pb dating of and grains yields ages around 4.1 Ga, indicating formation during the period. Specifically, maskelynite-pyroxene isochrons for ALH 84001 define a age of 4089 ± 73 Ma. For younger basaltic shergottites, which dominate the collection, ^40Ar/^39Ar dating of and separates provides ages typically between 150 and 600 Ma, though excess ^40Ar often complicates interpretation and requires careful step-heating to resolve trapped components. These ages cluster around ~200 Ma for many basaltic shergottites, aligning with Amazonian volcanism. Recent studies synchronize these Ar-Ar results with U-Pb phosphate ages, confirming mid-Amazonian for enriched shergottites at approximately 500-600 Ma. Ejection ages, marking the that launched meteorites from Mars, are determined using chronometers sensitive to shock-induced resetting. K-Ar dating, often via ^40Ar/^39Ar on maskelynite, shows partial resetting in shergottites, with apparent ages younger than crystallization but concordant with exposure histories, typically 1-20 Ma ago. For instance, in nakhlites and chassignites, K-Ar ages indicate ejection around 11 Ma, supported by partial degassing of radiogenic ^40Ar during the event. Pu-Xe chronometry, based on fissiogenic xenon isotopes from of extinct ^{244}Pu, provides complementary constraints; in ALH 84001, Pu-Xe ages overlap with K-Ar at ~4 Ga for early events but show younger resetting in shergottites around 200-500 Ma, demonstrating concordance with exposure timings. These methods reveal clustered ejection events, with most meteorites departing Mars in the last 20 Ma. Exposure ages quantify the duration of cosmic ray bombardment in space, calculated from accumulated cosmogenic nuclides. Concentrations of ^21Ne and ^38Ar in and whole-rock samples are measured, with production rates calibrated for stony compositions. Exposure ages for shergottites range from 1 to 15 Ma, while nakhlites and chassignites yield ~10-12 Ma, indicating multiple launch episodes. Production rates vary with depth in the pre-atmospheric body due to attenuation of secondary neutrons and protons. The depth-dependent production rate is modeled as P(z)=P0exp⁡(−ρzΛ),P(z) = P_0 \exp\left(-\frac{\rho z}{\Lambda}\right), where P(z)P(z) is the production rate at depth zz, P0P_0 is the surface rate, ρ\rho is the (~3 g/cm³ for Martian meteorites), and Λ≈150\Lambda \approx 150 g/cm² is the attenuation length for neutron-induced reactions in stony materials. This exponential model accounts for higher central production in larger meteoroids (>50 cm radius), ensuring accurate age calculations from nuclide gradients. Impact-induced resetting poses challenges, as shock pressures (20-60 GPa) during ejection cause partial of volatile elements like Ar, leading to intermediate ages between crystallization and ejection. In shergottites like NWA 2737, ^40Ar/^39Ar spectra show partial loss ~11 Ma ago, interpreted as shock heating to 300-500°C without full melt. Such resetting affects ~25% of samples, requiring cross-validation with multiple systems like (U-Th)/He in phosphates, which retain ejection signals better due to higher closure temperatures. These age determinations calibrate broader Martian chronologies, matching rover-derived crater counts for young volcanic surfaces. For example, Amazonian crystallization ages of shergottites (~200 Ma) align with estimates from crater counting for recent volcanism <100 Ma as of 2025, validating impact flux models.

Scientific Implications

Insights into Martian Geology

Martian meteorites provide key evidence for the ' mantle, which is depleted in aluminum and enriched in iron relative to . Parent magmas of shergottites, the most abundant group, exhibit low Al₂O₃ contents (typically 4-6 wt%) compared to terrestrial basalts, consistent with in a global magma ocean where aluminum was sequestered into high-pressure phases like majorite. This depletion, alongside elevated FeO (18-20 wt% in bulk silicate Mars), reflects early differentiation processes that concentrated iron in the . Hafnium-tungsten systematics in shergottites and other meteorites indicate core formation occurred rapidly, within the first 1-2 million years after Solar System accretion around 4.567 Ga, establishing a metallic core by approximately 4.5 Ga. The volcanic history of Mars, as sampled by meteorites, reveals episodic spanning billions of years. Ungrouped meteorites like NWA 7034/7533 contain clasts with crystallization ages up to 4.476 Ga, representing ancient volcanism shortly after crust formation. Nakhlites and chassignites crystallized around 1.3 Ga during the period, likely from sills or flows in a stable crustal environment. Shergottites, primarily basaltic, formed in the Amazonian era with ages less than 500 Ma (many 150-330 Ma), linking to prolonged activity in the volcanic province where depleted sources match impact-ejected materials from craters like . Crust-mantle differentiation occurred early, within 5-10 million years post-accretion, producing layered reservoirs without subsequent large-scale mixing. Meteorites primarily sample shallow depths of 10-50 km, including cumulates and crustal intrusions, as inferred from pyroxene thermometry and modeling of staging chambers near the Moho. The persistence of distinct isotopic signatures across groups indicates a stagnant lid regime with no evidence for or crustal recycling over 4.5 Ga. Hydrous minerals such as , , and iddingsite in nakhlites and shergottites record interaction with -rich fluids, suggesting a role for past surface or subsurface reservoirs. These phases, with contents up to 0.4 wt%, formed via low-temperature alteration, implying limited but widespread circulation or transient during the Noachian-Hesperian transition. Compositions of Gale crater basalts analyzed by Curiosity match aspects of shergottite geochemistry, including similar olivine (Mg# ~60-70) and pyroxene end-members, supporting a shared mantle-derived origin despite local variations in alkalis and silica. Perseverance findings in Jezero crater further align with meteorite-derived models of mafic volcanism, reinforcing interpretations of Mars' igneous evolution.

Potential Evidence of Life

In 1996, a team led by scientists announced potential evidence of ancient microbial in the Martian meteorite ALH 84001, based on features within its globules that formed approximately 3.9 billion years ago. These included polycyclic aromatic hydrocarbons (PAHs) concentrated in the globules, chains of nanocrystals resembling those produced by on , and compositions suggestive of biologically influenced precipitation. The PAHs were shown to be indigenous to the meteorite through contamination control experiments, with distributions correlating to the biogenic-like structures. Further analysis revealed elongated, worm-like nanoscale structures within the carbonates, measuring 0.2 to 0.5 μm in length, which were interpreted as possible fossilized remnants of Martian nanobacteria. The carbonate globules also displayed carbon isotope ratios (δ¹³C) ranging from +30‰ to +60‰, values that are heavy and atypical for biological fractionation processes on Earth. However, these interpretations faced significant scrutiny; studies demonstrated that the magnetite chains and PAHs could form abiotically through shock heating during the meteorite's ejection from Mars or via aqueous serpentinization of olivine in a hydrothermal environment. Additionally, the structures' sub-micron size is considered too small to accommodate the metabolic and reproductive machinery required for known life forms, favoring inorganic precipitation or mineral growth as explanations. Claims of biogenic features extended to other meteorites, such as Nakhla, where a 2001 study reported organic-rich halos surrounding iddingsite alteration veins, interpreted as possible microbial remnants from approximately 1.3 billion years ago. These findings were later debunked as terrestrial contamination, with microbial penetration documented to depths of several millimeters in samples collected shortly after the 1911 fall. No confirmed biosignatures have been identified in other Martian meteorites, such as Shergotty or the nakhlites. The scientific consensus today is that ALH 84001 and similar cases provide no definitive proof of past life on Mars, as all proposed biogenic indicators admit abiotic origins. Nonetheless, these investigations have refined criteria for astrobiological evidence, informing missions like the Perseverance rover, whose 2025 detection of organic carbon and redox features in Jezero Crater rocks echoes the meteorite debates without resolving them.

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