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

  • Book Review: Oxygen in the Solar System, Glenn MacPherson (Ed.)

    Lyon, Ian (The Meteoritical Society, 2008-01-01)
  • Magnetic classification of stony meteorites: 2. Non-ordinary chondrites

    Rochette, Pierre; Gattacceca, Jérôme; Bonal, Lydie; Bourot-Denise, Michèle; Chevrier, Vincent; Clerc, Jean-Pierre; Consolmagno, Guy; Folco, Luigi; Gounelle, Matthieu; Kohout, Tomas; et al. (The Meteoritical Society, 2008-01-01)
    A database of magnetic susceptibility (Chi) measurements on different non-ordinary chondrites (C, E, R, and ungrouped) populations is presented and compared to our previous similar work on ordinary chondrites. It provides an exhaustive study of the amount of iron-nickel magnetic phases (essentially metal and magnetite) in these meteorites. In contrast with all the other classes, CM and C show a wide range of magnetic material content, with a two orders of magnitude variation of Chi. Whether this is due to primary parent body differences, metamorphism or alteration, remains unclear. C3-4 and C2 yield similar Chi values to the ones shown by CK and CM, respectively. By order of increasing Chi, the classes with well-grouped Chi are: R << CO < CK is approximately equal to CI < Kak < CR < E is approximately equal to CH < CB. Based on magnetism, EH and EL classes have indistinguishable metal content. Outliers that we suggest may need to have their classifications reconsidered are Acfer 202 (CO), Elephant Moraine (EET) 96026 (C4-5), Meteorite Hills (MET) 01149, and Northwest Africa (NWA) 521 (CK), Asuka (A(+)-88198, LaPaz Icefield (LAP) 031156, and Sahara 98248 (R). Chi values can also be used to define affinities of ungrouped chondrites, and propose pairing, particularly in the case of CM and CV meteorites.
  • The Isheyevo meteorite: Mineralogy, petrology, bulk chemistry, oxygen, nitrogen, carbon isotopic compositions, and 40Ar-39Ar ages

    Ivanova, Marina A.; Kononkova, Natalia N.; Krot, Alexander N.; Greenwood, Richard C.; Franchi, Ian A.; Verchovsky, Alexander B.; Trieloff, Mario; Korochantseva, Ekaterina V.; Brandstatter, Franz (The Meteoritical Society, 2008-01-01)
    Isheyevo is a metal-rich carbonaceous chondrite that contains several lithologies with different abundances of Fe,Ni metal (7-90 vol%). The metal-rich lithologies with 5060 vol% of Fe,Ni metal are dominant. The metal-rich and metal-poor lithologies are most similar to the CBb and CH carbonaceous chondrites, respectively, providing a potential link between these chondrite groups. All lithologies experienced shock metamorphism of shock stage S4. All consist of similar componentsFe,Ni metal, chondrules, refractory inclusions (Ca, Al-rich inclusions [CAIs] and amoeboid olivine aggregates [AOAs]), and heavily hydrated lithic clastsbut show differences in their modal abundances, chondrule sizes, and proportions of porphyritic versus non-porphyritic chondrules. Bulk chemical and oxygen isotopic compositions are in the range of CH and CB chondrites. Bulk nitrogen isotopic composition is highly enriched in 15N (delta-15N = 1122). The magnetic fraction is very similar to the bulk sample in terms of both nitrogen release pattern and isotopic profile; the non-magnetic fraction contains significantly less heavy N. Carbon released at high temperatures shows a relatively heavy isotope signature. Similarly to CBb chondrites, ~20% of Fe,Ni-metal grains in Isheyevo are chemically zoned. Similarly to CH chondrites, some metal grains are Ni-rich (>20 wt% Ni). In contrast to CBb and CH chondrites, most metal grains are thermally decomposed into Ni-rich and Ni-poor phases. Similar to CH chondrites, chondrules have porphyritic and non-porphyritic textures and ferromagnesian (type I and II), silica-rich, and aluminum-rich bulk compositions. Some of the layered ferromagnesian chondrules are surrounded by ferrous olivine or phyllosilicate rims. Phyllosilicates in chondrule rims are compositionally distinct from those in the hydrated lithic clasts. Similarly to CH chondrites, CAIs are dominated by the hibonite-, grossite-, and melilite-rich types; AOAs are very rare. We infer that Isheyevo is a complex mixture of materials formed by different processes and under different physico-chemical conditions. Chondrules and refractory inclusions of two populations, metal grains, and heavily hydrated clasts accreted together into the Isheyevo parent asteroid in a region of the protoplanetary disk depleted in fine-grained dust. Such a scenario is consistent with the presence of solar windimplanted noble gases in Isheyevo and with its comparatively old K-Ar age. We cannot exclude that the K-Ar system was affected by a later collisional event. The cosmic-ray exposure (CRE) age of Isheyevo determined by cosmogenic 38Ar is ~34 Ma, similar to that of the Bencubbin (CBa) meteorite.
  • A study of ordinary chondrites by Mossbauer spectroscopy with high-velocity resolution

    Oshtrakh, M. I.; Petrova, E. V.; Grokhovsky, I.; Semionkin, V. A. (The Meteoritical Society, 2008-01-01)
    An improvement in the velocity resolution and quality of Mössbauer spectra has been applied to a group of ordinary chondrites. This improvement permitted us to carry out a more detailed study of the iron bearing phases in these samples than has previously been possible. Mössbauer spectra of 11 ordinary chondrites of L and H chemical groups were measured using 4096 channels and presented for further analysis in 1024 channels. Subspectra of the metal grains of several chondrites demonstrated the presence of at least two magnetic sextets related to the main Fe(Ni, Co) phases. Moreover, Mössbauer study of extracted metal grains from Tsarev L5 revealed three sextets and one singlet spectral components related to various alpha-Fe(Ni, Co), alpha'-Fe(Ni, Co), alpha2-Fe(Ni, Co), and gamma-Fe(Ni, Co) phases. Each subspectrum of olivine and pyroxene in Mössbauer spectra of ordinary chondrites was fitted by superposition of two quadrupole doublets related to M1 and M2 sites in minerals for the first time. An analysis of relative areas and Mössbauer hyperfine parameters was performed and some differences for L and H chondrites as well as for M1 and M2 sites were observed. Mössbauer parameters of troilite and oxidized iron were analyzed. In contrast to a previous study with 512-channel spectra, the presence of oxidized iron was found in all chondrites.
  • Yellow impact glass from the K/T boundary at Beloc (Haiti): XANES determination of the Fe oxidation state and implications for formation conditions

    Giuli, Gabriele; Eeckhout, Sigrid Griet; Koeberl, Christian; Pratesi, Giovanni; Paris, Eleonora (The Meteoritical Society, 2008-01-01)
    We determined the iron oxidation state and coordination number in five samples of yellow impact glass from the Cretaceous-Tertiary (K/T) boundary section at Beloc, Haiti, which formed as the result of impact melting during the Chicxulub impact event. The samples were analyzed by Fe K-edge XANES spectroscopy and the results were compared with published data on eight black impact glasses and one high Si-K impact spherule from the same impact layer. The pre-edge peak of our high-resolution XANES spectra displays evident variations indicative of significant changes in the Fe oxidation state, spanning a wide range from about 75 to 100 mole% Fe3+. Yellow K/T glasses have significantly higher Fe3+/(Fe2+ + Fe3+) ratios compared to black K/T impact glasses (from 20 to 75 mole% Fe3+) and high Si-K glass (20 mole% Fe3+). In particular, all the pre-edge peak data on these three types of impact glasses plot between two mixing lines joining a point calculated as the mean of a group of tektites studied so far (consisting of [4]Fe2+ and [5]Fe2+) to [4]Fe3+ and [5]Fe3+, respectively. Thus, the XANES spectra of the yellow K/T glasses can be interpreted as a mixture of [4]Fe2+, [5]Fe2+, [4]Fe3+, and [5]Fe3+. Our observations can be explained by a very large range of oxygen fugacity conditions during melt formation. Furthermore, there is a clear positive relationship between the Fe3+/(Fe2+ + Fe3+) ratio and the Ca content of these glasses, suggesting that the Fe oxidation state was influenced by the relative contribution of Ca-sulfate-and Ca-carbonate-bearing sedimentary rocks at the impact site.
  • Rosetta target asteroid 2867 Steins: An unusual E-type asteroid

    Weissman, Paul R.; Hicks, Michael D.; Abell, Paul A.; Choi, Young-Jun; Lowry, Stephen C. (The Meteoritical Society, 2008-01-01)
    ESAs Rosetta spacecraft will fly by main-belt asteroid 2867 Steins on September 5, 2008. We obtained new visible wavelength spectra of 2867 Steins on December 19, 2006 (UT), using the Palomar 5 m telescope and the facility Double Spectrograph. Two sets of spectra, taken ~3 h apart, one half of the rotation period for 2867 Steins, show it to be an E-type asteroid. The asteroid displays a 0.50 micrometer feature that is considered diagnostic of the E(II) sub-class, but is deeper than any previously observed E-type. This feature is most likely due to the presence of oldhamite (CaS) on the asteroids surface. Also, the observed Steins spectra are far redder than any other known E-types. There is potential evidence for heterogeneity on hemispheric scales, one side of the asteroid appearing to be significantly redder than the other. No known recovered meteorite sample matches the unusual spectra of 2867 Steins, but the closest analog would be similar to an enstatite achondrite (aubrite).
  • Observations and interpretations at Vredefort, Sudbury, and Chicxulub: Towards an empirical model of terrestrial impact basin formation

    Grieve, R. A. F.; Reimold, W. U.; Morgan, J.; Riller, U.; Pilkington, M. (The Meteoritical Society, 2008-01-01)
    The structural, topographic and other characteristics of the Vredefort, Sudbury, and Chicxulub impact structures are described. Assuming that the structures originally had the same morphology, the observations/interpretations for each structure are compared and extended to the other structures. This does not result in any major inconsistencies but requires that the observations be scaled spatially. In the case of Vredefort and Sudbury, this is accomplished by scaling the outer limit of particular shock metamorphic features. In the case of Chicxulub, scaling requires a reasoned assumption as to the formation mechanism of an interior peak ring. The observations/interpretations are then used to construct an integrated, empirical kinematic model for a terrestrial peak-ring basin. The major attributes of the model include: a set of outward-directed thrusts in the parautochthonous rocks of the outermost environs of the crater floor, some of which are pre-existing structures that have been reactivated during transient cavity formation; inward-directed motions along the same outermost structures and along a set of structures, at intermediate radial distances, during transient cavity collapse; structural uplift in the center followed by a final set of radially outward-directed thrusts at the outer edges of the structural uplift, during uplift collapse. The rock displacements on the intermediate, inward and innermost, outward sets of structures are consistent with the assumption that a peak ring will result from the convergence of the collapse of the transient cavity rim area and the collapse of the structural uplift.
  • Scanning electron microscopical and cross sectional analysis of extraterrestrial carbonaceous nanoglobules

    Garvie, Laurence A. J.; Baumgardner, Grant; Buseck, Peter R. (The Meteoritical Society, 2008-01-01)
    Carbonaceous nanoglobules are ubiquitous in carbonaceous chondrite (CC) meteorites. The Tagish Lake (C2) meteorite is particularly intriguing in containing an abundance of nanoglobules, with a wider range of forms and sizes than encountered in other CC meteorites. Previous studies by transmission electron microscopy (TEM) have provided a wealth of information on chemistry and structure. In this study, low-voltage scanning electron microscopy (SEM) was used to characterize the globule forms and external structures. The internal structure of the globules was investigated after sectioning by focused ion beam (FIB) milling. The FIB-SEM analysis shows that the globules range from solid to hollow. Some hollow globules show a central open core, with adjoining smaller cores. The FIB with an SEM is a valuable tool for the analysis of extraterrestrial materials, even of sub-micron "soft" carbonaceous particles. The rapid site-specific cross-sectioning capabilities of the FIB allow the preservation of the internal morphology of the nanoglobules, with minimal damage or alteration of the unsectioned areas.
  • Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite

    Busfield, A.; Turner, G.; Gilmour, J. D. (The Meteoritical Society, 2008-01-01)
    We have determined initial 129I/127I ratios for mineral concentrates of four enstatite meteorites and a eucrite. In the case of the enstatite meteorites the inferred ages are associated with the pyroxene-rich separates giving pyroxene closure ages relative to the Shallowater standard of Indarch (EH4, -0.04 +/- 0.67 Ma), Khairpur (EL6, -4.22 +/- 0.67 Ma), Khor Temiki (aubrite, -0.06 Ma), and Itqiy (enstatite achondrite, -2.6 +/- 2.6 Ma), negative ages indicate closure after Shallowater. No separate from the cumulate eucrite Asuka (A-) 881394 yielded a consistent ratio, though excess 129Xe was observed in a feldspar separate, suggesting disturbance by thermal metamorphism within 25 Ma of closure in Shallowater. Iodine-129 ages are mapped to the absolute Pb-Pb time scale using the calibration proposed by Gilmour et al. (2006) who place the closure age of Shallowater at 4563.3 +/- 0.4 Ma. Comparison of the combined 129I-Pb data with associated 53Mn ages, for objects that have been dated by both systems, indicates that all three chronometers evolved concordantly in the early solar system. The enstatite chondrites are offset from the linear array described by asteroid-belt objects when 53Mn ages are plotted against combined 129I-Pb data, supporting the suggestion that 53Mn was radially heterogeneous in the early solar system.
  • Petrology of Martian meteorite Northwest Africa 998

    Treiman, A. H.; Irving, A. J. (The Meteoritical Society, 2008-01-01)
    Nakhlite Northwest Africa (NWA) 998 is an augite-rich cumulate igneous rock with mineral compositions and oxygen isotopic composition consistent with an origin on Mars. This 456- gram, partially fusion-crusted meteorite consists of (by volume) ~75% augite (core composition Wo39En39Fs22), ~9% olivine (Fo35), ~7% plagioclase (Ab61An35) as anhedra among augite and olivine, ~3.5% low-calcium pyroxenes (pigeonite and orthopyroxene) replacing or forming overgrowths on olivine and augite, ~1% titanomagnetite, and other phases including potassium feldspar, apatite, pyrrhotite, chalcopyrite, ilmenite, and fine-grained mesostasis material. Minor secondary alteration materials include iddingsite associated with olivine (probably Martian), calcite crack fillings, and iron oxide/hydroxide staining (both probably terrestrial). Shock effects are limited to minor cataclasis and twinning in augite. In comparison to other nakhlites, NWA 998 contains more low-calcium pyroxenes and its plagioclase crystals are blockier. The large size of the intercumulus feldspars and the chemical homogeneity of the olivine imply relatively slow cooling and chemical equilibration in the late- and post-igneous history of this specimen, and mineral thermometers give subsolidus temperatures near 730 degrees C. Oxidation state was near that of the QFM buffer, from about QFM-2 in earliest crystallization to near QFM in late crystallization, and to about QFM + 1.5 in some magmatic inclusions. The replacement or overgrowth of olivine by pigeonite and orthopyroxene (with or without titanomagnetite), and the marginal replacement of augite by pigeonite, are interpreted to result from late-stage reactions with residual melts (consistent with experimental phase equilibrium relationships). Apatite is concentrated in planar zones separating apatite-free domains, which suggests that residual magma (rich in P and REE) was concentrated in planar (fracture?) zones and possibly migrated through them. Loss of late magma through these zones is consistent with the low bulk REE content of NWA 998 compared with the calculated REE content of its parent magma.
  • Two distinct assemblages of high-pressure liquidus phases in shock veins of the Sixiangkou meteorite

    Chen, M.; Xie, X. (The Meteoritical Society, 2008-01-01)
    Shock-produced complex veins, including earlier and later veins, are identified in the Sixiangkou L6 chondrite. The early vein is intersected by the late vein and consists of coarse-grained aggregates of ringwoodite, majorite, and lingunite, and fragments of olivine, pyroxene, plagioclase, metal, and troilite, as well as a fine-grained matrix of garnet, ringwoodite, metal, and troilite. The late vein mainly consists of a fine-grained matrix of garnet, magnesiowstite, metal, and troilite, as well as a small amount of coarse-grained aggregates. The amount of fine-grained matrix suggests that the late vein was nearly completely melted, whereas the early vein underwent partial melting. Both fine-grainedassemblages of garnet plus ringwoodite in the early vein and garnet plus magnesiowstite in the late veinare liquidus phases crystallized from shock-induced melt. Based on our understanding of the liquidus assemblages, the late vein experienced a higher pressure and temperature than the early vein.