Meteoritics & Planetary Science is an international monthly journal of the Meteoritical Society—a scholarly organization promoting research and education in planetary science. Topics include the origin and history of the solar system, planets and natural satellites, interplanetary dust and interstellar medium, lunar samples, meteors and meteorites, asteroids, comets, craters, and tektites.

Meteoritics & Planetary Science was first published in 1935 under the title Contributions of the Society for Research on Meteorites. In 1947, the publication became known as Contributions of the Meteoritical Society and continued through 1951. From 1953 to 1995, the publication was known as Meteoritics, and in 1996, the journal's name was changed to Meteoritics & Planetary Science or MAPS. The journal was not published in 1952 and from 1957 to 1964.

This archive provides access to Meteoritics & Planetary Science Volumes 37-44 (2002-2009).

Visit Wiley Online Library for new and retrospective Meteoritics & Planetary Science content (1935-present).

ISSN: 1086-9379


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Recent Submissions

  • The Zakłodzie enstatite meteorite: Mineralogy, petrology, origin, and classification

    Przylibski, T.; Zagożdżon, P.; Kryza, R.; Pilski, A. S. (The Meteoritical Society, 2005-01-01)
    The Zakłodzie meteorite was found in September 1998, about 40 km west of Zamość, in southeast Poland. Macroscopic and microscopic observations (in transmitted and reflected light), microprobe analyses, cathodoluminescence images, and X-ray diffraction data show that the meteorite is composed of clino- and orthoenstatite, two generations of feldspars, relict olivine (forsterite), a polymorph of SiO2 (apparently cristobalite), and opaque minerals: Fe-Ni alloy (kamacite and taenite), troilite, schreibersite, graphite, and sulfide (Mg, Mn, Fe)S, which is probably keilite. The texture is fine- to inequigranular of cumulate type, locally intergranular. The MgS-FeS thermometer indicates that the sulfides crystallized at ~580-600 degrees C. Thus, the Zakłodzie meteorite formed by the nearly complete melting of an enstatite chondrite protolith, probably at ~4.4 Ga; the process was likely caused by the decay of the 26Al nuclide in the planetesimal interior. The second stage of its evolution, which could have happened at ~2.1 Ga, involved partial re-melting of most fusible components, probably due to collision with another body. The structure, composition, and origin of the meteorite and its relation to the parent rock indicate that Zakłodzie may represent a primitive enstatite achondrite.
  • Author Index

    The Meteoritical Society, 2005-01-01
  • Subject Index

    The Meteoritical Society, 2005-01-01
  • The Meteoritical Bulletin No. 89

    Russell, S. S.; Zolensky, M.; Righter, K; Folco, L.; Jones, R.; Connolly, H. C.; Grady, M. M.; Grossman, J. N. (The Meteoritical Society, 2005-01-01)
    This Bulletin lists 1768 meteorites, bringing the total known meteorites to over 30,000 at 30,907. Of these, 1010 are from Antarctica, 569 from Africa, 92 from Asia (83 of which are from Oman), 85 from North America, one from South America and 11 from Europe. The Bulletin reports seven falls (Benguerir, Bukhara, Kasauli, Maigatari-Danduma, Oum Dreyga, Rahimyar Khan, and San Michele). Noteworthy specimens include 20 lunar meteorites, four Martian meteorites, two pallasites, three mesosiderites, and two Bencubbin-like meteorites. Additional information can be found at http://meteoriticalsociety.org/bulletin/database.html.
  • Meteorites from Botswana

    Sokol, A. K.; Bischoff, A. (The Meteoritical Society, 2005-01-01)
    In 1999, the first meteorites from Botswana were recovered. Most samples (seven) were purchased from natives in the small village of Kuke. We suggest that these samples were found close to Kuke in the Kalahari desert. As reported by the finder, the other four samples were recovered during geological field work in various areas of Botswana in April (Mabe), September (Kalahari 008 and 009), and November 1999 (Matisama). Kalahari 008 and Kalahari 009 were found close to the small village of Kuke and are chemically and petrographically different lunar rocks. However, we suggest that both samples represent distinct lithologies of one meteoroid and that the lunar sample broke apart at the find site. The other nine samples are H-group ordinary chondrites. Based on different petrologic types, the degrees of shock metamorphism and weathering pairing of most samples can be ruled out. We conclude that only Kalahari 004 and Kalahari 005 are paired.