Introduction to Martian Meteorites

Until that moment, Martian Meteorites are the only Martian samples in our hands to develop such Analytical Strategies.

The geochemical properties of Laramie ferrihydrite are shared by some samples of altered chondritic and Martian meteorites.

We show that the source localities for many martian meteorites are capable of producing sufficient redox nutrients to sustain up to millions of sulfate-reducing microbial cells per kilogram rock via radiolysis alone, comparable to cell densities observed in many regions of Earth's deep subsurface.

Martian atmospheric neon (Ne) has been detected by Viking and also found as trapped gas in Martian meteorites, though its abundance and isotopic composition have not been well determined.

Until successful completion of sample-return missions from Mars, Martian meteorites are currently the only samples of the red planet available for study in terrestrial laboratories and comparison with in situ data.

It should be noted that the Phobos regolith is expected to contain a small amount of materials delivered from Mars, which may be physically and chemically different from any Martian meteorites in our collection and thus are particularly precious.

Significance Using spacecraft data and elemental abundances derived from martian meteorites, earlier studies set a paradigm of a volatile- and water-rich Mars relative to Earth.

Analyses of Martian meteorites using the extinct hafnium–tungsten (Hf–W) 16 radioisotopic system, which is sensitive to the timing of core formation, have indicated that the 17 Martian core formed within a few million years of the solar system itself.

Martian meteorites are the only available samples that can be directly measured to constrain the geological evolution of Mars.

Martian meteorites have valuable information about past geological processes on Mars.

We report the largest variation in δ34S yet found in martian meteorites (−13.

Observations of the Martian surface from orbiting spacecraft and in situ landers and rovers, as well as analyses of Martian meteorites in terrestrial laboratories, have consistently indicated that Mars is a sulfur-rich planet.

We evaluated the mineralogical, geochemical, and physical properties of the Balos cove basalts (BCB) from the island of Santorini and compared them to Martian meteorites, Mars rover surface measurements, and other verified Martian analogues obtained from the International Space Analogue Rockstore (ISAR).

The African population comprises an abundance of stony meteorites with high percentages of rare meteorites of the world collection: Martian meteorites (62%), Ureilites (51%), Rumuruti (59%), Lunar (47%), and HED (46%).

Using our results, we revisited the REE geochemistry of chassignites, a grouplet of Martian meteorites.

Therefore in order to understand the concentrations of volatiles in the crust, it is vital to first constrain the volatile budget of the Martian interior, the preeruptive volatile content of Martian magmas, and evidence within the Martian meteorites for magmatic degassing.

Calcium pyroxenes in martian meteorites are associated with secondary evaporite phases, including sulfates, chlorides, and perchlorates, suggesting the pyroxene may have been altered in saline solutions.

Here we present an alternative model composition for Mars that avoids such an assumption and is based on data from Martian meteorites and spacecraft observations.

Martian meteorites have been dated precisely and quantitatively, but the launch sites are currently unknown.

Here we quantify for the first time the potential importance of aeolian abrasion as a mechanism for releasing trapped methane from within rocks, by coupling estimates of present day surface wind abrasion with the methane contents of a variety of Martian meteorites, analogue terrestrial basalts and analogue terrestrial sedimentary rocks.

Martian meteorites, such as Northwest Africa (NWA) 6963, can be excellent materials for understanding the present and past of Mars, as part of the records of the planet's evolution is preserved in these extraterrestrial rocks.

Direct evidence of fluid-rock interaction on Mars comes from iddingsite alteration veins found in martian meteorites.

These impacts have produced impact-generated Mars ejecta, and a fraction of this debris is delivered to Earth as Martian meteorites.

Among those, hydrated minerals testify to past aqueous weathering processes that can be precisely studied in Martian meteorites such as NWA 7533/7034.