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Tadeusz Andrzej PRZYLIBSKI Andrzej Sylwester PILSKI Pawe&#x; Przemys&#x;aw ZAGOZ
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ON Ryszard KRYZA 《Meteoritics & planetary science》2003,38(6):927-937
Abstract— We review the petrology of Baszkówka, present new microprobe data on mineral constituents, and propose a model for surface properties of the parent body consistent with these data. The low shock index and high porosity of the Baszkówka L5 chondrite mean that considerable primary textural and petrographic detail is preserved, allowing insight into the structure and evolution of the parent body. This meteorite formed in a sedimentary environment resembling that in which pyroclastic rocks are deposited. The origin of the component chondrules, achondritic fragments (mostly olivine and pyroxene aggregates), chondritic‐achondritic aggregates, and compound chondrules can be explained by invoking collision of 2 melted or partially melted planetesimals, each covered with a thin crust. This could have happened at an early stage in the evolution of the solar system, between 1 and 2 Myr after its origin. The collision resulted in the formation of a cloud containing products of earlier magmatic crystallization (chondrite and achondrite fragments) from which new chondrules were created. Particle collision in this cloud produced fragmented chondrules, chondritic‐achondritic aggregates, and compound chondrules. Within this low‐density medium, these particles were accreted on the surface of the larger of the planetesimals involved in the collision. The density of the medium was low enough to prevent grain‐size sorting of the components but high enough to prevent the total loss of heat and to enable the welding of fragments on the surface of the body. The rock material was homogenized within the cloud and, in particular, within the zone close to the planetesimal surface. The hot material settled on the surface and became welded as molten or plastic metal, and sulfide components cemented the grains together. The process resembled the formation of welded ignimbrites. Once these processes on the planetesimal surface were completed, no subsequent recrystallization occurred. The high porosity of the Baszkówka chondrite indicates that the meteorite comes from a near‐surface part of the parent body. Deeper parts of the planetesimal would have been more massive because of compaction. 相似文献
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In my former articles published in this Bulletin§ and in Science§§ (Chinese), I have attempted to show that the early possible date of using zinc in China can be traced since Han Dynasty (201 B. C.—200 A. D.), and 相似文献
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J. M. PAQUE J. R. BECKETT H. A. ISHII A. ALÉON‐TOPPANI D. S. BURNETT N. TESLICH Z. R. DAI J. P. BRADLEY 《Meteoritics & planetary science》2009,44(5):665-687
Abstract— We used focused ion beam thin section preparation and scanning transmission electron microscopy (FIB/STEM) to examine the interfacial region between spinel and host melilite for spinel grains in type B1 inclusions from the Allende and Leoville carbonaceous chondrites. Boundary clinopyroxenes decorating spinel surfaces have compositions similar to those of coarser clinopyroxenes from the same region of the inclusion, suggesting little movement after formation. Host melilite displays no anomalous compositions near the interface and late‐stage minerals are not observed, suggesting that boundary pyroxenes did not form by crystallization of residual liquid. Allende spinels display either direct spinel‐melilite contact or an intervening boundary clinopyroxene between the two phases. Spinel‐melilite interfacial regions in a Leoville B1 are more complex, with boundary clinopyroxene, as observed in Allende, but also variable amounts of glass, secondary calcite, perovskite, and an Mg‐, Al‐, OH‐rich and Ca‐, Si‐poor crystalline phase that may be a layered double hydrate. One possible scenario of formation for the glass veins is that open system alteration of melilite produced a porous, hydrated aggregate of Mg‐carpholite or sudoite + aluminous diopside that was shock melted and quenched to a glass. The hydrated crystalline phase we observed may have been a shocked remnant of the precursor phase assemblage, but is more likely to have formed later by alteration of the glass. In the mantle, boundary clinopyroxenes may have been crystallized from Ti‐rich liquids formed by the direct dissolution of perovskite and an associated Sc‐Zr‐rich phase or as a reaction product between dissolving perovskite and liquid. In the core, any perovskite and associated Ti‐enriched liquids that may have originally been present disappeared before the growth of boundary clinopyroxene, and the observed boundary clinopyroxene may have nucleated and grown from the liquid, along with the larger core clinopyroxene. 相似文献
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Neil B. McLaughlin 《山地科学学报》2011,(5)
Geohazards appear to be increasing in frequency globally. It is of necessity to actively manage these natural hazards to minimize loss of life and property. From an early warning perspective, this paper stresses the potential fatal flood hazard represented by the huge volume of water in Tianchi Lake, the unique geography of Changbai Mountain, and the limited flood control ability in the upstream of the Songhua River. Northeast Asian countries should keep a watchful eye on the Changbai volcano cooperatively,... 相似文献
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Jrme ALON Alexander N. KROT Kevin D. MCKEEGAN Glenn J. MACPHERSON Alexander A. ULYANOV 《Meteoritics & planetary science》2005,40(7):1043-1058
Abstract— Oxygen isotopes have been measured by ion microprobe in individual minerals (spinel, Al‐Ti‐diopside, melilite, and anorthite) within four relatively unaltered, fine‐grained, spinel‐rich Ca‐Al‐rich inclusions (CAIs) from the reduced CV chondrite Efremovka. Spinel is uniformly 16O‐rich (Δ17O ≤ ?20‰) in all four CAIs; Al‐Ti‐diopside is similarly 16O‐rich in all but one CAI, where it has smaller 16O excesses (‐15‰ ≤ Δ17O ≤ ?10‰). Anorthite and melilite vary widely in composition from 16O‐rich to 16O‐poor (‐22‰ ≤ Δ17O ≤ ?5‰). Two of the CAIs are known to have group II volatility‐fractionated rare‐earth‐element patterns, which is typical of this variety of CAI and which suggests formation by condensation. The association of such trace element patterns with 16O‐enrichment in these CAIs suggests that they formed by gas‐solid condensation from an 16O‐rich gas. They subsequently experienced thermal processing in an 16O‐poor reservoir, resulting in partial oxygen isotope exchange. Within each inclusion, oxygen isotope variations from mineral to mineral are consistent with solid‐state oxygen self‐diffusion at the grain‐to‐grain scale, but such a model is not consistent with isotopic variations at a larger scale in two of the CAIs. The spatial association of 16O depletions with both elevated Fe contents in spinel and the presence of nepheline suggests that late‐stage iron‐alkali metasomatism played some role in modifying the isotopic patterns in some CAIs. One of the CAIs is a compound object consisting of a coarse‐grained, melilite‐rich (type A) lithology joined to a fine‐grained, spinel‐rich one. Melilite and anorthite in the fine‐grained portion are mainly 16O‐rich, whereas melilite in the type A portion ranges from 16O‐rich to 16O‐poor, suggesting that oxygen isotope exchange predated the joining together of the two parts and that both 16O‐rich and 16O‐poor gaseous reservoirs existed simultaneously in the early solar nebula. 相似文献
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王水辰 《中国海洋大学学报(自然科学版)》1995,(3)
作者根据Ｋｅｅｌｉｎｇ等人提出的１９７０～１９８８年大气ＣＯ２含量随时间变比进行统计，指出大气ＣＯ２含量按指数变化递增。据此．对近年大气ＣＯ２含量进行预测，到２０５０年时将增至４５４×１０－６，较目前增加约３０％。由于大气ＣＯ２分压上升，导致ＣＯ２向海洋转移、作者采用Ｌｉ提出的指数变化模式，以Ｈｏｌｌａｎｄ给出的海水中无机碳逗留时间８．０×１０４年代入计算。到２０５０年时，海水碳酸盐系统仅可容纳来自大气的ＣＯ２１．１×１０１０ｔ。因此必须引起人们控制ＣＯ２向大气的排放。鉴于计算过程中未考虑海水有机生物体的影响及颗粒ＣａＣＯ３对缓冲ＣＯ２所作贡献，因此，实际情况会好于本文计算结果。 相似文献
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S. B. SIMON D. J. JOSWIAK H. A. ISHII J. P. BRADLEY M. CHI L. GROSSMAN J. ALÉON D. E. BROWNLEE S. FALLON I. D. HUTCHEON G. MATRAJT K. D. McKEEGAN 《Meteoritics & planetary science》2008,43(11):1861-1877
Abstract— Among the samples returned from comet 81P/Wild 2 by the Stardust spacecraft is a suite of particles from one impact track (Track 25) that are Ca‐, Al‐rich and FeO‐free. We studied three particles from this track that range in size from 5.3 × 3.2 μ to 15 × 10 μ. Scanning and transmission electron microscopy show that they consist of very fine‐grained (typically from ?0.5 to ?2 μ) Al‐rich, Ti‐bearing and Ti‐free clinopyroxene, Mg‐Al spinel and anorthite, with trace amounts of fine perovskite, FeNi metal and osbornite (TiN) grains. In addition to these phases, the terminal particle, named “Inti”, also contains melilite. All of these phases, with the exception of osbornite, are common in refractory inclusions and are predicted to condense at high temperature from a gas of solar composition. Osbornite, though very rare, has also been found in meteoritic refractory inclusions, and could have formed in a region of the nebula where carbon became enriched relative to oxygen compared to solar composition. Compositions of Ti‐pyroxene in Inti are similar, but not identical, to those of fassaite from Allende inclusions. Electron energy loss spectroscopy shows that Ti‐rich pyroxene in Inti has Ti3+/Ti4+within the range of typical meteoritic fassaite, consistent with formation under reducing conditions comparable to those of a system of solar composition. Inti is 16O‐rich, with δ18O?δ17O?‐40%0, like unaltered phases in refractory inclusions and refractory IDPs. With grain sizes, mineralogy, mineral chemistry, and an oxygen isotopic composition like those of refractory inclusions, we conclude that Inti is a refractory inclusion that formed in the inner solar nebula. Identification of a particle that formed in the inner solar system among the comet samples demonstrates that there was transport of materials from the inner to the outer nebula, probably either in a bipolar outflow or by turbulence. 相似文献
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