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Supplement Abstracts.Fm Abstracts for the 61st Annual Meeting of the Meteoritical Society Item Type Article; text Citation Abstracts for the 61st Annual Meeting of the Meteoritical Society. Meteoritics & Planetary Science, 43(S7), 15-178 (2008). DOI 10.1111/j.1945-5100.2008.tb00711.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 28/09/2021 00:01:36 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656517 Meteoritics & Planetary Science 43, Nr 7, Supplement, A15–A178 (2008) http://meteoritics.org Abstracts 5316 5030 ROSETTA FLYBY TARGET ASTEROID (2867) STEINS: AN VARIETIES OF CARBON MINERALS IN ANTARCTIC ENSTATITE ACHONDRITE ANALOGUE CARBONACEOUS CHONDRITES BY TEM AND THEIR P. A. Abell 1, 2, P. R. Weissman3, M. D. Hicks3, Y. J. Choi3, and S. C. Lowry3. IMPLICATIONS 1Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ Junji Akai1, Takayuki Aoki2, and Hikaru Ohtani1. 1Department of Geology, 85719, USA. E-mail: [email protected]. 2NASA Johnson Space Center, Fac. Sci., Niigata University, Niigata, Japan. 2Asahi Carbon Co., Niigata, Houston, TX 77058, USA. 3Jet Propulsion Laboratory, 4800 Oak Grove Japan. Drive, Pasadena, CA 91109, USA. A variety of fine-grained carbonaceous materials are contained in Introduction: On September 5, 2008, the European Space Agency’s carbonaceous chondrite (CC) matrix. However, Antarctic meteorites have not Rosetta spacecraft will fly by the main-belt asteroid (2867) Steins enroute to always been examined in detail. Eight Antarctic carbonaceous chondrites its primary target, comet 67P/Churyumov-Gerasimenko. Given that little Asuka-882094 (CO3), Yamato-86751 (CV3), Yamato-790992 (CO3), information was known about Steins prior to its selection as a Rosetta flyby Yamato-81020 (CO3), Yamato-74662 (CM2), Yamato-86720 (CM2), target in 2004, a ground-based observational campaign was undertaken to Yamato-793321 (CM2), Belgica-7904 (CM2 or “CI1”), and Allende and ensure that good constraints of the asteroid’s physical characteristics were Murchison were systematically examined in more detail. We developed a measured before the encounter. sample separation procedure of chemical dissolution, using HF (48, nitric Observations: CCD spectroscopic (~0.33 to 0.93 µm) reflectance acid) and aqua regia, at 348 K for 30 minutes. observations of asteroid (2867) Steins were obtained to further investigate its TEM used is JEM-2010 (JEOL) and JEM-200CX with EM-SHH4 compositional characteristics and determine the most likely meteoritic (heating holder). Zinc powder was used for temperature calibration. Multi- analogue. Given that the rotation period of this asteroid was previously slice TEM simulation (MssC) was carried out. determined to be ~6.05 h [1], two sets of spectra were collected over an ~3 h Nano-diamond and “carbonaceous globules” were found from seven interval in order to obtain data on each hemisphere of the asteroid. An Antarctic chondrites. Diamond grains are clearly more abundant than well- examination of the spectra demonstrates that the asteroid has a significant crystallized graphite in the CC. About the origin of nano-diamond, a presolar absorption feature located near 0.50 µm, and a red spectral slope at longer CVD formation model has been widely accepted (e.g., [1]). Although some wavelengths up through 0.92 µm. In addition, previous investigators have possibility of its formation on parent body is also suggested [2], the results of determined that the albedo of Steins is ~0.30–0.55 [2, 3]. This suggests that it this study suggest that the presolar origin is more likely than the parent-body has spectral properties most consistent with the E-type asteroids, which are origin. As Nakamura-Messenger et al. (2006) [3] suggested, carbonaceous known for their high albedos [4]. globules may be primitive carbon material formed in the outermost cold Interpretation: Some E-type asteroids are distinguished from other E regions of protoplanetary disks. The results of this study indicate that subtypes by spectral absorption features located near 0.50 µm and 0.96 µm. nanodiamond and carbonaceous globules are very common constituents in E(II)-type asteroids (64) Angelina and (3103) Eger have been observed to CC. We carried out heating and cooling experiments of carbonaceous have features located near 0.50 µm [5], and both of these asteroids have high globules in electron microscopic observation mainly to examine their thermal albedo values [6, 7, 8]. The preferred mineralogical interpretation is that stability and changes. Neither graphitization nor significant changes in shape these features are produced as a result of the presence of the calcium sulfide and size were observed in heating at 773 K. ED patterns show that the globule mineral, oldhamite (CaS) on the surface of these asteroids [9, 10]. Oldhamite remains amorphous even after heating. This result suggests that these is characterized by two absorption features located near 0.50 µm and 0.96 µm carbonaceous globules can survive strong thermal metamorphism. Detailed that are probably produced by trace amounts of a bivalent ion, such as Fe2+, TEM observation of boundary part of the doughnut-like globules was carried that has been substituted into the sulfide instead of Ca2+. In addition, out. The carbonaceous globules are similar in size to the smallest bacteria in oldhamite is present only in highly reduced mineral assemblages such as the recent Earth environments. If much carbonaceous globules were supplied aubrite (enstatite achondrite) meteorites [11, 12]. onto the Earth surface in the early stage of its evolution, we suggest the Conclusions: A comparison of laboratory spectra of aubrite ALH possibility that they played some role in the birth and/or early evolution of 78113 to the Steins data suggests that there is a plausible similarity between life on the Earth. this meteorite and the asteroid in terms of albedo and absorption features. Well crystallized graphite with 2H and 3R polytypes was also found Hence the most likely meteoritic analogue to Steins is an aubrite with a mainly from CV3 and CO3 chondrites, whereas poorly crystallized graphite spectrally significant amount of sulfide (e.g., CaS) present in its assemblage. was found mainly from CM2 chondrites. Characteristic carbon structures References: [1] Weissman et al. 2007. Astrononomy & Astrophysics similar to tetrahedral carbon onion etc. were found from a CM2 chondrite. 466:737–742. [2] Fornasier et al. 2006. Astrononomy & Astrophysics 449: Finally, correspondence of carbon mineral types to petrological classification L9–L12. [3] Lamy et al. 2006. BAAS 38, #59.09. [4] Barucci et al. 2005. of CC is summarized. We will discuss more about the implications. Astrononomy & Astrophysics 430:313–317. [5] Fornasier and Lazzarin. References: [1] Daulton T. et al. 1996. Geochimica et Cosmochimica 2001. Icarus 152:127–133. [6] Tedesco et al. 1989. Asteroids II. pp. 151– Acta 60:4853–4872. [2] Kouchi A. et al. 2005. The Astrophysical Journal 1161. [7] Veeder et al. 1989. The Astronomical Journal 97:1211–1219. [8] 626:L129–L132. [3] Nakamura-Messenger K. et al. 2006. Science 314:1439– Benner et al. 1997. Icarus 130:296–312. [9] Burbine et al. 2002. Meteoritics 1442. & Planetary Science 37:1233–1244. [10] Gaffey and Kelley. 2004. Abstract #1812. 35th LPSC. [11] Keil. 1989. Meteoritics 24:195–208. [12] Fogel. 1997. Meteoritics & Planetary Science 32:577–591. A15 © The Meteoritical Society, 2008. Printed in USA. A16 71st Meeting of the Meteoritical Society: Abstracts 5046 5117 HIGH-PRESSURE PHASE RELATIONS OF Ca,Na- WATER IN TERRESTRIAL PLANETS ALUMINOSILICATE, CAS PHASE, WITH IMPLICATION TO F. Albarede. Ecole Normale Supérieure, 69007 Lyon, France. E-mail: SHOCKED MARTIAN METEORITES [email protected]. M. Akaogi1, M. Haraguchi1, M. Yaguchi1, K. Nakanishi1, and H. Kojitani1. Department of Chemistry, Gakushuin University, 1-5-1 Mejiro, Toshima-ku, Mars and the Moon are dry and inactive deserts. Their interiors came to Tokyo 171-8588, Japan. E-mail: [email protected]. rest within one billion years of accretion. Venus, although internally very active, has a dry inferno for a surface. In contrast, the Earth is tectonically Introduction: Ca,Na-aluminosilicate (Ca1-x,Nax)Al4-xSi2+xO11 named active and largely covered by a deep ocean. The strong gravity field of large CAS phase, a high-pressure silicate with hexagonal barium-ferrite structure, planets allows for an enormous amount of gravitational energy to be released, was found in heavily shocked Martian meteorites by Beck et al. [1]. High causing the outer part of the planetary body to melt (magma ocean), thus pressure experiments demonstrated that the CAS phase was synthesized in helping retain water on the planet. The analysis of K/U and 87Sr/86Sr ratios in high pressure mineral assemblages of anorthite [2] and oceanic sediments [3], planetary objects further demonstrates that the inner solar system lost up to and the CAS phase was also found as a liquidus phase in melting experiments 95% of its K and Rb. Planets in such an environment cannot contain much of mid-oceanic ridge basalt [4]. We have examined high-pressure high- water (~20 ppm). temperature phase relations of CaAl4Si2O11 and those in the system The relationship between terrestrial element abundances and CaAl4Si2O11-NaAl3Si3O11, using a multianvil press. We have also measured condensation temperatures shows that the Earth and the
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