Lunar and Planetary Science XXXVI (2005) sess112.pdf PRINT-ONLY: METEORITES Alexeev V. A. Ustinova G. K. Meteorite Data on the Solar Modulation of Galactic Cosmic Rays and an Inference on the Solar Activity Influence on Climate of the Earth [#1012] Meteorite data on the galactic cosmic rays, the solar activity, and temperature variations in the Earth’s atmosphere lead to the conclusion that the solar activity may be important factor exerting the influence upon the climate of the Earth. Badjukov D. D. Brandstätter F. Kurat G. Libowitzky E. Raitala J. Ringwoodite-Olivine Assemblages in Dhofar 922 L6 Melt Veins [#1684] Melt veins in the L6 chondrite Dhofar 922 contain olivine-ringwoodite assemblages. Compositions of these co-existing olivine and ringwoodite correspond to the formation of the assemblages at 1200°C and 12.7 GPa. Moggi-Cecchi V. Pratesi G. Mancini L. NWA 1052 and NWA 1054: Two New Primitive Achondrites from North West Africa [#1808] NWA 1052 and 1054 are two meteorites containing olivine, low- and high-Ca pyroxene, plagioclase, Fe-Ni, troilite, Cl-apatite and chromite. The texture and EMPA data on olivine and low- and high-Ca pyroxene suggest a classification as acapulcoites. Fogel R. A. An Analysis of the Solvus in the CaS-MnS System [#2395] Solution modeling of experimental datasets for the CaS-MnS system indicate serious inter- and intra-dataset inconsistencies. This calls into question the use of MnS in CaS and CaS in MnS as geothermometers with current datasets. New experimental data for this system are presented for 1100°C. Hua X. Wang Y. Hsu W. Sharp T. G. Fremdlinge in Chondrules and Matrix of the Ningqiang Carbonaceous Chondrite [#1762] A large number of Fremdlinge are found in chondrules and matrix of Ningqiang. Their mineral assemblages are similar to those in Allende CAIs. Their formation was a common phenomenon, closely associated with formation of CAIs and chondrules. Ivanova M. A. Nazarov M. A. Brandstätter F. Moroz L. V. Ntaflos Th. Kurat G. Mineralogical Differences Between Metamorphosed and Non-Metamorphosed CM Chondrites [#1054] As compared to normal CM chondrite, Dhofar 955, the metamorphosed CM chondrites, Dhofar 225 and Dhofar 735 are characterized by a lack of tochilinite, and a lack of P-rich sulfides. These features could be due to thermal metamorphism. Ivliev A. I. Kuyunko N. S. Skripnik A. Ya. Nazarov M. A. Thermoluminescence Studies of Carbonaceous Chondrites [#1065] The purpose of the present paper was to study carbonaceous chondrite metamorphism using the TL-device of the Vernadsky Institute. Kurat G. Varela M. E. Zinner E. Silicate Inclusions in the Kodaikanal IIE Iron Meteorite [#1814] II-E iron meteorites are particularly interesting because they contain an exotic zoo of silicate inclusions including some chemically strongly fractionated ones. Here we present preliminary findings in our study of Kodaikanal silicate inclusions. Lavrentjeva Z. A. Lyul A. Yu. Shubina N. A. Kolesov G. M. REE and Some Other Trace Elements Distributions of Mineral Separates in Atlanta (EL6) [#1011] REE and some other trace element distributions of mineral separates in Atlanta (EL6) are presented. Lunar and Planetary Science XXXVI (2005) sess112.pdf Lorenz C. A. Ivanova M. A. Kurat G. Brandstätter F. FeO-rich Xenoliths in the Staroye Pesyanoe Aubrite [#1612] The nine FeO-rich mineral and lithic clasts, corresponding to H- and carbonaceous chondrites, were found in the Staroye Pesyanoe aubrite. It indicates that flux of interplanetary dust onto aubrite parent body was different from that of Earth and HED. Miyamoto M. Jones R. H. Koizumi E. Mikouchi T. Verification of a Model to Calculate Cooling Rates in Olivine by Consideration of Fe-Mg Diffusion and Olivine Crystal Growth [#1610] We developed a model to analyze chemical zoning in olivine based on Fe-Mg diffusion during olivine crystal growth to obtain the cooling rate. We verify this model by using Fe-Mg zoning in olivine produced by dynamic crystallization experiments. Okazaki R. Nakamura T. Origin and Thermal History of Lithic Materials in the Begaa LL3 Chondrite [#1533] Origin and thermal history of unusually large lithic materials found in the Begaa LL3 chondrite is discussed based on the major/minor element abundances, oxygen isotopic ratios, and rare earth element abundances. Pletchov P. Yu. Zinovieva N. G. Latyshev N. P. Granovsky L. B. Evaluation of the Crystallization Temperatures and Pressures for Clinopyroxene in the Parental Bodies of Ordinary Chondrites [#1041] Thermo- and barometry of clinopyroxene in ordinary chondrites indicates that, regardless of the chemical groups and petrological types of chondrites, they crystallized from chondritic melts at pressures of >0 kbar. Skála R. Císařová I. Crystal Structure of Troilite from Chondrites Etter and Georgetown [#1284] Crystal structure of troilites from chondrites Etter and Georgetown is consistent with that reported earlier for troilite or its synthetic analogues. Studied troilites are slightly cation-deficient. The crystals represent the inversion twins. Takeda H. Yamaguchi A. Otsuki M. Ishii T. New Achondrites with High-Calcium Pyroxene and Its Implication for Igneous Differentiation of Asteroids [#1298] We report two new achondrites, which contain more augite than previously described. Combined with data of silicate inclusions in IAB and IIE irons, we propose that augites are important component in partial melts of chondritic source materials. Wasson J. T. Matsunami Y. Rubin A. E. Possible Formation of IVA Irons by Impact Melting and Reduction of L-LL Chondrite Materials [#1511] The oxygen-isotope composition of silicates in IVA irons indicates an origin from L-LL chondritic materials. This requires appreciable reduction. We suggest that melting and reduction resulted from an impact onto a porous primitive chondritic body. Zinovieva N. G. Pletchov P. Yu. Latyshev N. P. Granovsky L. B. Physicochemical Conditions of Clinopyroxene Crystallization in the Parental Bodies of Ordinary Chondrites [#1038] Thermobarometry of pyroxenes in ordinary chondrites indicates that they crystallized from chondritic melts, first, under significant pressures in large parental bodies and then continued to crystallize in much smaller bodies (~9 kbar, R~750–850 km). .