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Thursday, July 30, 1998 EARLY CHRONOLOGY and PLANETARY PROCESSES 2:00 P.M Thursday, July 30, 1998 EARLY CHRONOLOGY AND PLANETARY PROCESSES 2:00 p.m. Ussher Theatre Chairs: J. D. Gilmour G. Srinivasan Kita N. T.* Nagahara H. Togashi S. Morishita Y. New Evidence of Aluminum-26 from an Ferrous-Oxide-rich Chondrule in Semarkona (LL3.0) Srinivasan G.* Goswami J. N. Bhandari N. Search for Extinct Aluminum-26 in the Piplia Kalan Eucrite Pravdivtseva O. V.* Hohenberg C. M. Brazzle R. H. Isotopic Record of Shock Metamorphism in the Richardton H5 Chondrite Hohenberg C. M.* Brazzle R. H. Pravdivtseva O. V. Meshik A. P. Iodine-Xenon Chronometry: The Verdict Whitby J. A.* Gilmour J. D. Turner G. In Situ Analysis of the Iodine-Xenon System in a Saharan EH3 Chondrite Burkland M. K.* Swindle T. D. The Thermal Retentive Nature of the Iodine-Xenon System in the Ordinary Chondrite Bjurböle: Implications for the Iodine-Xenon System as a Chronometer of Early Solar System Events Kunz J.* Allègre C. J. Terrestrial Xenology and Early Evolution of Earth Turner G.* Burnard P. Harrison D. The Plane Truth About Primordial Noble Gases on Earth Ozima M.* Podosek F. A. Formation Interval of the Earth from Iodine-129/Iodine-127 and Plutonium-244/Plutonium-238 Systematics and Missing Xenon Hohenberg C. M. Thonnard N.* Kehm K. Meshik A. P. Berryhill A. Glenn A. Active Capture of Volatives: Implication for Planetary and Atmospheric Xenon Manuel O.* Isotopic Ratios in Jupiter Confirm Intrasolar Diffusion Hill L. C. Jr.* The Urey Hypothesis Revisited: Molecular Genetics and Contemporary Chronologies NEW EVIDENCE OF ALUMINUM-26 FROM A FEO-RICH CHONDRULE IN SEMARKONA (LL3.0). N. T. Kita1, H. Nagahara2, S. Togashi1, and Y. Morishita1, 1Geological Survey of Japan, 1-1-3 Higashi, Tsukuba 305- 8567, Japan, 2Geological Institute, University of Tokyo, Hongo, Tokyo 113-0033, Japan. Introduction: The 26Mg excess from the decay of of Japan for SIMS analyses [6]. The primary ion of 26Al (half life = 0.73 Myr) were found from numbers – O2 was focused to a diameter of 3–6 µm for Al-Mg of Al-rich chondrules in UOCs [1–3]. The initial analyses and 15 µm for Fe-Ni analyses. The typical 26 27 –5 Al/ Al abundance of these chondrules ( ~ 1¥ 10 ) precision of single analyses was 3–7 ‰ for Mg iso- –5 are significantly lower than those of CAIs (~ 5¥ 10 ), topes and 5 ‰ for Ni isotopes. suggesting that the formation of chondrules took place Results and Discussion: The Al/Mg ratios of the at least 1–2 Myr after the CAIs formation. The Al-Mg mesostasis was as high as 160, and a clear 26Mg ex- age information was not available for the majority of cess was observed up to 14 ± 5 ‰ (2s). The results chondrules in UOCs because they do not contain high from 6 data show a linear trend on the Al-Mg iso- 60 60 (Al/Mg) phases for the Al-Mg study. The Fe- Ni chron diagram with the slope corresponding to system (half life = 1.5 Myr) will be an useful chro- (26Al/27Al) = (1.16 ± 0.25) ¥ 10–5. The result indicates nometer, though the estimates of the initial solar that CH4 formed (1.56 ± 0.23) Myr after CAIs forma- 60 56 ( Fe/ Fe) ratios are uncertain in the range between tion. The present Al-Mg results imply that Type-II –6 –8 10 and 10 [4]. chondrules formed contemporary with more refractory In this work we focused on Type-II POP chon- Al-rich chondrules. The 56Fe/58Ni ratios of olivine 26 26 drules from Semarkona (LL3.0) for Al– Mg and were between 2300 and 2800. The mean value of 21 60 60 Fe– Ni study using SIMS. These chondrules contain analyses (d60Ni = –0.04 ± 0.99 ‰, 2s) do not show FeO-rich olivine and pyroxene, set in a Si, Al, Fe -rich any detectable 60Ni excess. The upper limit of mesostasis with quenched crystals [5]. Therefore, they 60Fe/56Fe ratio in CH4 is calculated to be 1.4 ¥ 10–7. are suitable samples containing high Al/Mg and high Using the Al-Mg relative age, the upper limit of the Fe/Ni phases. 60Fe/56Fe ratio at the time of CAI formation is esti- Samples and Experiments: A Type II chondrule mated to be 3.3 ¥ 10–7. This value is similar to the “CH4” (0.5 ¥ 0.8 mm) was examined in a polished recent estimate of less than 2 ¥ 10–7 using the FeS thin section of Semarkona (USMN 1805-9). The from an H4 chondrite with known U-Pb age [4]. sample contains 100–300 µm olivine phenocrysts (Fo References: [1] Srinivasan G. et al. (1996) LPS = 88 ~ 83), which are normally zoned at the rim (Fo = XXVII, 1257–1258. [2] Russell S. S. et al. (1996) Sci- 75). Pyroxene grains are smaller (30–100 µm) and ence, 273, 757–762. [3] Russell S. S. et al. (1997) zoned (En = 77 ~ 83, Ws = 1 ~ 5). The composition of LPS XXVIII, 1209–1210. [4] Shukolyukov A. and mesostasis is rich in Na, Al, and Si (65–70% SiO , 4– 2 Lugmair G. W. EPSL, 119, 159–166. [5] Jones R. H. 8% Na O, and 12–18 % Al O ). The fibrous quench 2 2 3 (1996) GCA., 60, 3115–3138. [6] Kita N. T. et al. crystals with high Fe, Mg, and Ca (pyroxene ?) are abundant in the mesostasis. However, several areas (1998) Antarct. Meteorite Res., 11, 105–123 larger than 5 µm are free of quenched crystals and show Al/Mg ratios of as high as ~200 (EPMA data). These area were selected for the SIMS analyses. We used the Cameca IMS-1270 at the Geological Survey SEARCH FOR EXTINCT ALUMINUM-26 IN PIPLIA KALAN EUCRITE. G. Srinivasan, J. N. Goswami, and N. Bhandari, Earth Science and Solar System Division, Physical Research Laboratory, Ahmedabad 380 009, India ([email protected]). The short-lived radionuclide 26Al (halflife ~0.7 clase and pyroxene crystals were studied for Al-Mg Ma) was postulated as a heat source for the early composition using Cameca ims-4F ion microprobe. melting and differentiation of planetesimals by Urey Back scattered electron image of PK-97-1 was used to in 1955 [1]. Since then the presence of 26Mg excess avoid pyroxene grains (hot spots of Mg) present (26Mg*) due to the decay of 26Al has been established within plagioclase crystals. The results of this study in Ca-Al-rich Inclusions (CAIs) and chondrules [2-7]. shows that 27Al/24Mg value ranges from 3000-6000 in The presence of extinct 26Al in Semarkona clast plagioclase with 26Mg* values varying from 6‰ to chondrule with initial 26Al/27Al ~ 8 × 10–6 suggests 48‰. Our data yields initial (26Al/27Al) value of (7.0 26 –7 that Al abundance was sufficient to produce incipi- ± 2.0) ×10 (2sm). This study provides for the first ent melting of well insulated bodies of chondritic time a very strong evidence for the presence of live composition [7], although the relationship between 26Al at the time of formation of eucrite Piplia Kalan basaltic achondrites and igneous clasts in chondrites and suggests a time interval of ~5 Ma between the is not clear. Several attempts over the last twenty five formation of CAIs and this meteorite. The contribu- years to look for extinct 26Al in eucrites, angrites, tion of cosmogenic 26Al in this meteorite with an ex- mesosiderites [8-11], plagioclase-rich clast from posure age of 23 Ma [16] is <0.1% of the measured North Haig ureilite [12], and “microgabbro” clast in excess. Our results confirm the antiquity of this mete- Parnallee [13] have remained unsuccessful, although orite as indicated by the Sm-Nd ages and suggest that in several cases upper limits for 26Al abundance have 26Al could have played an important role as a heat been estimated. If the heat for melting of parent bod- source in the formation of differentiated meteorites. ies of eucrites was generated from 26Al decay then References: [1] Urey H. (1955) Proc. Natl. some evidence for its presence must be seen in differ- Acad. Sci. US, 41, 127. [2] Lee T et al. (1976) Geo- entiated meteorites provided the parent bodies cooled phys. Res. Lett., 3, 109. [3] MacPherson G. J. et al. on a time scale of few million years. The recently (1995) Meteoritics, 30, 365. [4] Srinivasan G. et al. fallen eucrite Piplia Kalan [14] has been shown to be (1996) LPSC XXVII, 1257. [5] Srinivasan G. et al. extremely old based on Sm-Nd and Pu-Xe ages (1996) Meteoritics and Planet. Sci., 31, A133 [6] [15,16]. We have measured Al-Mg composition in Russell S. S. et al. (1996) Science, 273, 757. 4571. several plagioclase crystals from Piplia Kalan to fur- [7] Hutcheon I. D. and Hutchison R. (1989) Nature, ther investigate the role of 26Al in early melting of 337, 238. [8] Schramm D. et al. (1970) EPSL, 10, 44. parent bodies of differentiated meteorites. [9] Bernius et al. (1991) LPSC XXII, 93. [10] Lug- One thin section (PK-97-1) was documented mair G. W. and Galer S. J. G. (1992) GCA, 56, 1673. using a Cameca SX electron microprobe (NASA [11] Hsu W. and Crozaz G. (1996) GCA, 60. [12]. Johnson Space Center, Houston) and it exhibits both Davis A. et al. (1988) LPSC XIX, 251. [13] Kennedy coarse grained and fine grained features. The major A. et al. (1992) EPSL, 113, 191. [14] Shukla A. et al. minerals are plagioclase (An95), Ca-rich and Fe-rich (1997) Meteoritics and Planet. Sci., 32, 611. [15] pyroxenes, and chromite and ilmenite are also present Kumar A et al.
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