lvuna
B-7904 Y-793321 Y-86720 CM mean
CM cv CR co CK Kobe
5
1015 20
N/Mn (atomic ratio)
25 30
Figure 6.5 SIMn vs AlllVln diagram for studied meteorites along with some representative members of other carbonaceous chondrite groups. Data for CI, CM, CO, CV, CR and one Karoonda (CK) are from
McSween and Rjchardson (1977), another Karoonda (CK) from Fitzgerald (1979) and Kobe (CK)
from Oura et al. (2002).6.6 References
Akai, J. 1988. lncompletely transformed serpentine-type phyllosilicates in the matrix of Antarctic
CM2 chondrites. Geochimica et Cosmochimica Acta 52, 1593-1599.
Akai, J. 1990. Mineralogical evidence of heating events in Antarctic carbonaceous chondrites 86720 and Y-82162. Proceedings ofthe NIPR Symposium on Antarctic Meteorites 3, 55-68.
Akai, J. 1992. T-T-T diagram of serpentine and saponite, and estimation of metamorphic heating degree of Antarctic carbonaceous chondrites. Proceedings of the NIPR Symposium on Antarctic Meteon'tes 5, 120-135.
Akai, J. 1994. Void structures in olivine grains in thermally metamorphosed Antarctic carbonaceous chondrite B-7904. Proceedings ofthe NIPR Symposium on Antarctic Meteorites 7, 94-1OO.
Akai, J. and Sekine, T. 1994. Shock effects experiments on serpentine and thermal metamorphic conditions in Antarctic carbonaceous chondrite. Proceedings ofthe NIPR Symposium on Antarctic Meteorites 7, 1O1-109.
Akai, J.; Tari, S.; Tanaka, H. 1996, New descriptions and re-examinations on thermal metamorphisms
in several Antarctic CM2 carbonaceous chondrites: Preliminary reports. 2Ist Symposium on
Antarctic Meteorites, National lnstitute ofPolar Research, Tokyo, p. 1 -•3.Anders, E and Grevesse, N. 1989, Abundances of the elements: Meteoritic and solar. Geochimica et
Cosmochimica Acta 53,197-214.
Ash, R. D. and Pillinger, C. T. 1992. The effects of Saharan weathering on light element contents of various primitive chondrites (abstract). Meteoritics 27, 199.
Ball, M.C. and Taylor, H. F. W. 1963. Dehydration of chrysotile in air and under hydrothermal conditions. Mineral. Mag. 33, 467-482.
Beck, P.; Quirico, E.; Montes-Hernandez, G.; Bonal, L.; Bollard, J.; Onhous-Daunay, F.-R.; Howard,
K. T.; Schmitt, B.; Brissaud, O.; Deschamps, F.; Wunder, B.; Guillot, S. 2010. Hydrous
mineralogy of CM and CI chondrites from infrared spectroscopy and their relationship with low albedo asteroids. Geochimica et CosmochimicaActa 74, 4881-4892.Bevan, A. W. R; Bland, P. A.; Jull, A, J. T. 1998. Ed. M. M. Grady , Meteorites: Flux with Time and lmpact Effects. Geol. Soc., London, P. 59-73.
Bischoff, A. and Metzler, K. 1991. Mineralogy and petrography of the anomalous carbonaceous chondrites, Yamato-86720, Yamato-82162 and Belgica-7904. Proceedings of the NIPR
Symposium on Antarctie Meteorites, Tokyo, Japan, 4, 226-246.Bland, P. A.; Zolensky, M. E.; Benedix, G. K.; Sephton, M. A. 2006. Weatheimg of chondritic
meteorites. Irt Meteorites and the early solar system II, edited by Lauretta D. S. and McSween H.Y, Tucson, AZ: The University ofArizona Press. p. 853-867.
Brearly, A,J.; Hutcheon, I.D. and Browning, L. 2001. Compositional zoning and Mn-Cr systematic in
carbonates from the Y-791198 CM2 carbonaceous chondrite. Lunar and planetary science
conference, 32, 1458pdf.Brindley, G. W. and Hayashi, R. 1965. Mechanism of formation of forsterite and enstatite from serpentine. Mineral. Mag. 35,189-195.
Brindley, G. W. and Zussman, J. 1957. Stmctural study of the thermal transformation of serpentine minerals to forsterite. Amer. Miner. 42, 461-474.
Browning, L. B.; McSween, Jr. H. Y. and Zolensky, M. E. 1996. Correlated alteration effects in CM carbonaceous chondrites. Geochimica et Cosmochimica Acta 60, 2621-2633.
Buddhue, J. D. 1957. The oxidation and weathering of meteorites. Albuquerque, NM: The University
ofNew Mexico, P.161.
Choe, W. H.; Huber, H.; Rubin, A. E.; Kallemeyn, G. W.; Wasson, J. T. 2010. Compositions and
taxonomy of 15 unusual carbonaceous chondntes. Meteoritics & Planetary Science 45, 531-554.Clayton, R. N. and Mayeda. 1999. 0xygen isotope studies ofcarbonaceous chondrites. Geochimica et Cosmochimica Acta 63, 2089-2104.
Clayton, R. N.; Mayeda, T. K.; Kojima H.; Weisberg M. K.; Prinz, M. 1997. Hydration and
dehydration in carbonaceous chondrites (abstract). Lunar Planet. Sci. 28, 239-240.Cloez, S. 1864. Note sur la composition chimique de la pierre meteoritique d'Orgueil. Compt. R. Acad.
Sci. Paris, 58, 986-988.
Dennison, J. E.; Lingner, D. W.; Lipschutz, M. E, 1986. Antarctic and non-Antarctic meteorites from different populations. Nature 319, 390-393.
Ebihara, M.; Shinonaga, T.; Nakahara, H.; Kondoh, A.; Miyamoto, M.; Kojima, H. 1989. profiles of halogen abundance and integrated intensity of hydration band near 3 pm in ALH
77231, Antarctic L6 chondrite. ln Differences between Antarctic and non-Antarctic meteorites, edited by Koeberl C. and Cassidy W. A. LPI Technical Report 90-OI. Houston, Texas: Lunar and Planetary lnstitute. p. 32-37.Eiler, J. M. and Kitchen, N. 2004. Hydrogen isotope evidence for the origin and evolution of the carbonaceous chondrites. Geochim. Cosmochim. Acta 68, 1395-141 1.
Fitzgerald M. J. 1979. The chemical composition and classification of the Karoonda meteorite.
Meteoritics 14, 109-115.
Friedrich, J. M.; Wang, M-S.; Lipschutz, M. E. 2002. Comparison ofthe trace element composition of Tagish Lake with other primitive carbonaceous chondrites. Meteoritics & Planet. Sci. 37, 677-686.
Gibson, .E. K...and Bogard,.D. D. 1..978,..(I eM. Qal alterations ofthe Holbrook chondrite resulting from terresuial weathering. Meteoritics 13, 277-289.
Gounelle, M, and Zolensky, M. E. 2001. A terrestrial origin for sulphate veins in CII chondrites.
Meteoritics & Planet. Sci. 36, l321-1329.
(]irimm, R, E. and McSween, H. Y. Jr. 1989. Water and thermal evolution of carbonaceous chondrite parent bodies, Icarus 82, 244-280.
Hiroi, T.; Pieters, C. M.; Zolensky, M. E.; Lipschutz, M. E. 1993. Evidence of thermal metamorphism on the C, G, B and F asteroids. Science 261, 1016-1018.
Hiroi, T.; Pieters, C. M.; Zolensky, M. E.; Lipschutz, M. E. 1994. Possible thermal metamorphism on
the C, G, B and F asteroids detected from their reflectance spectra in comparison with
carbonaceous chondrites. Proceedings ofthe NIPR Symposium on Antarctic Meteorites, lapan, 7,230-243.
Hiroi, T.; Pieters, C. M.; Zolensky, M. E.; Lipschutz, M. E. 1996. Possible thermal metamorphism on the C, G, B and F asteroids seen from the O.7, 3, and UV absorption strengths in comparison with carbonaceous chondrites. Meteoritics & Planetary Science 31, 321-327.
Hiroi, T.; Zolensky, M.E.; Pieters, C. M. 1997. Characterization of unusual CVCM7CR meteorites from reflectance spectroscopy. Proceedings qfthe 28th Lunar and Planetary Science Conference,
Abstract #1463.
Huber, H.; Rubin, A. E.; Kallemeyn, G. W.; Wasson, J. T. 2006. Siderophile-element anomalies in CK carbonaceous chondrites: lmplications for parent-body aqueous alteration and terrestrial weathering of sulfides. Geochimica et Cosmochimica Acta 70, 4019-4037.
Ikeda, Y. 1992. An overview of the research consonium, "Antarctic carbonaceous chondrites with CI
affmities, Yamato-86720, Yamato-82162 and Belgica-7904". Proceedings of the National
Institute ofPolar Research Symposium on Antarctic Meteorites, lapan, 5, 49-73.Ivanova, M. A.; Lorenz, C.A.; Nazarov, M. A.; Brandstaetter, F.; Franchi, I. A.; Moroz, L.V,; Clayton,
R. N.; Bychkov, A. Y. 2010. Dhofar 225 and Dhofar 735: relationship to CM2 chondrites and metamorphosed carbonaceous chondrites, Belgica-7904 and Yamato-86720. Meteoritics &
Planetary Science 45, 1108-1123.
Jarosewich, E.; Clarke Jr., R. S.; Barrows, J. N. 1987. The Allende meteorite reference sample. Smiths.
Contn'b. Earth Sci. 27, 1-49.
Kallemeyn, G. W. and Wasson, J. T. 1981. The compositional classification of chondrites-I. The carbonaceous chondrite group. Geochim. Cosmochinz. Acta 45, 1217-1230.
Kallemeyn, G. W.; Rubin, A. E.; Wang, D. and Wasson, J. T. 1989. 0rdinary chondrites: Bulk
compositions, classification, lithophile-element fractionations, and composition-petrographic type relationships. Geochim. Cosmochim. Acta 53, 2747-2767.Kallemeyn, G. W.; Rubin, A. E.; Wasson, J. T. 1994. The compositional classification of chondrites:
VI. The CR carbonaceous chondrite group. Geochimica et Cosmochimica Acta 58, 2873-2888.
Kimura, M. and lkeda, Y. 1992. Mineralogy and petrology of an unusual Belgica-7904 carbonaceous chondrite: genetic relationship among the components. Proceedings of the NIPR Symposium on Antarctic Meteorites 5, 74-1 19.
Kitajima, F.; Nakamura, T.; Takaoka, N.; Murae, T. 2e02. Evaluating the thermal metamorphism of
CM chondrites by using the pyrolytic behavior of carbonaceous macromolecular matter.
Geoehimica et CosmochimicaActa 66, 163-172.
Kojima, H. and Yamaguchi, A. 2008. Meteorite Newsletter Vol. 16. Antarctic Meteorite Research Center, National institute ofPolar Research, Tokyo, Japan.
Kojima, H.; ikeda Y.; Yanai, K. 1984, The alteration of chondmles and matrices in new Antarctic carbonaceous chondrites. Memoirs ofthe National Institute ofPolarResearch 35, 184-199.
Langenauer, M. and Krahenbuhl, U. 1993. Halogen contamination in Antarctic H5 and H5 chondntes and relation to sites ofrecovery. Earth andPlanetary Scienee Letters 120, 431-442.
Lipschutz, M. E.; Zolensky, M. E.; Sue Bell, M. 1999. New petrographic and trace element data on thermally metamorphosed carbonaceous chondrites. Antarctic Meteorite Research 12, 57-80.
Lodders, K. 2003. Solar system abundances and condensation temperatures of the elements.
Astrophys. 1. 591, 1220-1247.
Lodders, K. and Fegley, Jr. B. 1998. The Planetary Scientist's Companion, Oxford University press,
New York, USA, P. 314-316.
Mayeda, T. K. and Clayton, R, N. 1998. 0xygen isotope effects in serpentine dehydration. Lunar andPlaneta7y Science 29, abstract #1405.
McGarvie, D. W.; Wright, I. P.; Grady, M. M.; Pillinger, C. T.; Gibson, E. K. Jr.. 1987. A stable carbon isotopic study oftypes 1 and 2 carbonaceous chondntes. Memoirs ofthe National Institute ofpolar research 46,179-195.
McSween, H, Y. 1979. Alteration in CM carbonaceous chondrites inferred from modal and chemicai variations in matrix. Geochimica et Cosmochimiea Acta 43, 1761-1770.
McSween, H. Y. and Richardson, S. M. 1977. The composition of carbonaceous chondrites matrix.
Geochimica et Cosmochimica Acta 41, 1 145-1 161.
McSween, H. Y., Sears, D. W. G. and Dodd, R. T. 1988. Thermal metamorphism in meteorites and
the early solar system, edited by J. F. Kenidge and M. S. Mathews, 102-1 13, Univ. Arizona Press,Tucson, Arizona, USA.
Meteoritical Bulletin Database. 2012. The meteoritical society, Tucson, Arizona, USA
(http:11meteoriticalsociety.org, last updated on January 1O, 2012).
Metzler, K. and Bischoff, A. 1990. Petrography and chemistry of accretionary dust mantles in the
CM-chondrites Y-791 198, Y-793321, Y-74662 and ALHA831OO-indications for nebula process.
Proceedings ofthe NIPR Symposium on Antaren'c Meteorites 15, 198-200.
Metzler, K.; Bischoff, A.; St6ffler, D. 1992. Accretionary dust mantles in CM chondrites: Evidence for solar nebula processes. Geochimica et Cosmochimica Acta 56, 2873-2897.
Miyamoto, M. 1991a. Differences in the degree of weathering between Antarctic and non-Antarctic meteorites inferred from infrared diffuse reflectance spectra. Geochimica et Cosmochimica Acta 55, 89-98.
Miyamoto, M. 1991b. Thermal metamorphism of CI and CM carbonaceous chondrites: An internal
heating model, Meteoritics, 26,1 1 1-1 15.Miyamoto, M.; Fuji, N.; Takeda, H. 1981. 0rdinary chondrite parent body: an internal heating model, Proc. Lunar Planet Sci., 12B, 1145-1152.
Nakamura, T. 2005. Post-hydration thermal metamorphism of carbonaceous chondrites, J. MineraL Petrol. Sci., 100, 260-272.
Nakamura, T. 2006. Yamato 793321 CM chondrite: Dehydrated regolith material of a hydrous
asteroid, Earth Planet Sci. Letters 242, 26-38.Nakato, A.; Nakamura, T.; Kitajima F.; Noguchi, T. 20e8. Evaluation of dehydration mechanism
during heating ofhydrous asteroids based on mineralogical and chemical analysis ofnaturally and experimentally heated CM chondntes, Earth Planets Space, 60, 855-864.Naraoka, H.; Mita, H. ; Komiya, M.; Yoneda, S.; Kojima, H.; Shimoyama, A. 2004, A chemical sequence of macromolecular organic matter in the CM chondrites. Meteoritics & Planetary
Science 39, 401-406.Naraoka, H.; Shimoyama, A.; Matsubaya, O.; Harada, K. 1997. Carbon isotopic compositions of
Antarctic carbonaceous chondrites with relevance to the alteration and existence oforganic matter.Geochemical loumal 3 1, 155-168.
Ohtsuka, K; Sekiguchi, D.; Kinoshita, J.; Watanabe, I.; Ito, Y.; Arakida, H.g Kasuga, T. 2006. Apollo asteroid 2005 UD: split nucleus of (3200) Phaethon? Astron. Astrophys. 450, L25-L28.
Oura, Y.; Ebihara, M.; Yoneda, S.; Nakamura, N. 2002. Chemical composition of the Kobe meteorite:
Neutron-induced prompt gamma-ray analysis study. Geochem. J. 36, 295-307.
Oura, Y.; Takahashi, C.; Ebihara, M. 2004. B and Cl abundances in Antarctic chondrites: A PGA study. Antarctic Meteorite Research 17,172-184.
Paul, R, L. 1995. The use of element ratios to elminate analytical bias in cold neutron prompt gamma-ray activation analysis. 1. Radioanal. Nuel. Chem. 191, 245-256.
Presper, T.; Kurat, G.; Koeberl, C.; Palme, H.; Maurette, M. 1993. Elemental depletions in Antarctic micrometeorites and Arctic cosmic spherules: Comparison and relationships (abstract). 24th Lunar and Planetary Science Conference. p. 1 177-1 178.
Rowe, M, W.; Clayton, R. N.; Mayeda, T. K. 1994. 0xygen isotopes in separated components of CI
and CM meteorites. Geochimica et CosmochimicaActa 58 5341-5347.
'
Rubin, A. E.; Trigo-Rodriguez J. M.; Huber, H.; Wasson, J. T. 2007. Progressive alteration of CM carbonaceous chondrites, Geochimica et Cosmochimica Acta 71, 2361-2382.
Shimoyama, A.; Komiya, M.; Harada, K. 1991. Releqse of organic compounds from some Antarctic
CI and CM chondrites by laboratory heating. Proceedings ofthe NIPR Symposium on Antarctic
Meteorites 4, 247-260.Takeda, H,; Wooden, J. L.; Mori, H.; Delaney, J. S.; Prinz, M.; Nyquist, L. E. 1983. Comparison of Yamato and Victoria Land polymict eucrites: A view from mineralogical and isotopic studies.
Proceedings of the 14th Lunar and Planetary Science Conference. Journal of Geophysical
Research 88, B245-B256.
Tomeoka, K. 199e. Mineralogy and petrology of Belgica-7904: A new kind of carbonaceous
chondrites from Antarctica. Proceedings ofthe NIPR Symposium on Antarctic Meteorites, lapan, 3, 40-54.Tonui, E. K,; Zolensky, M. E.; Lipschutz, M. E. 2002. Petrology, mineralogy and trace element
chemistry of Yamato-86029, Yamato-793321 and Lewis Cliff-853321: Aqueously altered and
heating events. Antarctic Meteorite Research 15, 38--58.Tonui, E. K.; Zolensky, M. E.; Lipschutz, M. E.; Wang, M.; Nakamura, T. 2003. Yamato-86029:
Aqueously altered and thermally metamorphosed CI-1ike chondrite with unusual textures.
Meteoritics & Planetary Science 38, 269-295.
Tyburczy, J. A.; Frisch, B; Ahrens, T. J. 1986. Shock-induced volatile loss from a carbonaceous chondrite: implications for planetary accretion. Earth and Planetary Science Letters 80, 201-207.
Wang, M. and Lipschutz, M. E. 1998. Thermally metamorphosed carbonaceous chondrites from data for thermally mobile trace elements. Meteoritics & Planetary Science 33, 1297-1302.
Wiik, H. B. 1956. The chemical composition of some stony meteorites. Geochim. Cosmochim. Acta 9,
279-289.
Wolf, S. F. and Lipschutz, M. E. 1995. Chemical studies of H chondrites 6. Antarcticlnon-Antarctic compositional differences revisited. J. Geophys. Res. 100, 3335-3349.
Yanai, K,; Kojima, H,; Haramura, H. 1995. Catalog of the Antarctic meteorites collected from
December 1969 to December 1994, with special reference to those represented in the collections ofthe National lnstitute ofPolar Research, Tokyo, Japan, p. 44-76.Zanda, B.; Hewins, R. H.; Bourot-Denise, M.; Bland, P. A. and Albarede F. 2006. Formation of solar nebula reservoirs by mixing chondritic components. Earth Planet. Sci. Lett. 248, 650-660.
Zanda, B.; Le Guillou, C.; Hewins, R. H. 2009. The relationship between chondmles and matrix in chondrites. in: 72nd Annual Meeting ofthe Meteoritical-Society, Nancy, France.
Zolensky, M.; Abell, P; Tonui, E. 2005. Metamorphosed CM and CI carbonaceous chondrites could
be from the breakup of the same earth-crossing asteroid. 36`h Lunar and Planetary Seience
Conference, Abstract # 2084.Summary
This study evaluated the nondestructive and multi-elemental analysis of primitive carbonaceous
chondntes (CI and CnvC2) using neutron activation analysis ovM), especially neutron-induced
prompt gamma-ray analysis (PGA), for studying their chemical alteration history. To determine the chemical oomposition of CI and CMIC2 chondrites accurately by SPGA, neutron absorption, neutron scattering and gamma-ray attenuation were evaluated. A study performed by using GSJ-JB-2, as a meteorite analogue, mixed with oxalic acid (Ji[-contaming one) resulted in analytical sensitivity (count rate per unit mass) increases with increasing the matrix H concentration. With about 2 massO/o ofH, the sensitivity was enh. anced by about 80/o relative to a sample with OO/o mass ofH, which is within themarginal range of uncertainty due to the reproducibility of SPGA at JAEA. Evaluation of the
sensitivity change with increasing disk-shaped sample mass (or thickness) yielded no apparent enhancement of the sensitivity for any of the studied elements for the disk mass range of 400 mg to 1 g (corresponding thickness of2 to 5 mm). The sensitivity was decreased for thick samples because ofneutron absorption inside the samples and this change ofsensitivity could be ignored with a sample mass of up to O.4 g. Therefore, it was concluded that a sample mass ofCI and CM/C2 chondrites of up to O.4 g can be reliably anaiyzed by SPGA to avoid sensitivity change.Since enhancement of the element sensitivity was reported for hydrogenous disk-shaped sample by previous studies, which was not in agreement with our study at JRR-3M of Japan Atomic Energy Agency (JAEA), this effect was explicitly studied theoretically by PHITS code calculation as well as experimentally by using a cylindrical PTFE sample holder. The experimental sensitivity variation
with disk thickness observed at JRR-3M of JAEA could be explained by PHITS simulation by
consideimg both elastic and inelastic neutron scattering inside the hydrogenous disk sample, The overall agreement between experiment and PHITS calculation was generally good.MPGA system at JAEA was characterized for elemental analysis of geological and
cosmochemical samples. Using the optimized procedures of MPGA, primitive carbonaceous
chondntes were analyzed. It was shown that some elements which could not be determined by SPGA, dug to the spectral interference or lower sensitiyity, could be determined by MPGA. Comparison of SPGA and INtff'GA showed that MPGA could substantially reduce the background level, especially for hydrogenous samples relative to 'SPGA, which opens up a possibility to use lower energy prompt gamma rays ofsome trace elements for their quantification. As an example, with MPGA, Mg contents could be detemined with reasonable consistency with their corresponding recommended values in geological and cosmochemical samples by carefu11y selecting suitable coincident prompt gamma-ray energy pairs, which is difficult to detemine by SPGA. MPGA was also applied to a hydrogenous meteorite, Ivuna, which contains H at 20/o mass level, and it was concluded that MPGA detectionlimits for most of the elements studied could be reduced by up to one order of magnitude when compared with SPGA detection limits under the present experimental conditions.
Combining elemental abundances ofthe studied primitive carbonaceous chondrites determined by SPGA and INAA, the chemical composition of the studied meteorites were reported. The detailed chemical composition of the Antarctic CI chondrite, Y-980115, became fmstly available from this
study. The 1arge deviations of the abundances of Ti and H of Y-980115 from non-Antarctic CIs
(Orgueil, Ivuna and Alais) indicate that this Antarctic CI chondrite had experienced nebular andlor parent body processes to alter the primitive chemical composition. The bulk chemical compositions of B-7904 and Y-86720 indicate that they were related to CM chondrites, although oxygen isotopic compositions were nearly simi1ar to CI chondrites. The depletion trend of the thermally mobile and highly volatile elements in the metamorphosed Antarctic chondrites indicated that B-7904 is severely altered while Y-793321 is least altered, with Y-86720 being in-between. This study enabled us to understand that some asteroids experienced post-accretional heating, presumably due to impact, which had caused their volatile element loss during thermal events.Acknowledgments
I would 1ike to express my sincere gratitude and honor to my supervisor Professor Mitsuru
Ebihara for his invaluable gutidance, advice and inspiration throughout the progress of this research. I am also gratefu1 to Dr. Yasuji Oura, Dr. Hideo Harda and Dr. Shiro Kubuki for their carefu1 review and constructive comments on the thesis. I also would 1ike to thank Assistant Professor Naoki Shirai for his help and advice on different issues. I am very gratefu1 to Dr. Yosuke Toh, Dr. Tadahiro Kin and Dr. Hideaki Matsue ofJapan Atomic Energy Agency, Tokai for their help during experiment and simulation study. I would 1ike to thank Dr. Takashi Sano ofNational Museum ofNature and Science, Tokyo for his kind permission to use his laboratory. I am also gratefu1 to many people who helped me over the years, particularly the members ofthis laboratory Yoshihiro Hidaka and Wee Boon Siong for a lot of enjoyable discussion.I am gratefu1 to National lnstitute ofPolar Research (NIPR), Japan and other national museums of