Mathematics – Logic
Scientific paper
Sep 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995metic..30q.568r&link_type=abstract
Meteoritics, vol. 30, no. 5, page 568
Mathematics
Logic
2
Accretion, Hot, Autometamorphism, Metamorphism, Prograde, Thermal, Meteorites, Conquista, Quenggouk, Tieschitz
Scientific paper
The extensive recrystallization of type-6 OC has been interpreted as having resulted either from prograde thermal metamorphism of initially cold, unequilibrated material [1,2] or from autometamorphism due to slow cooling of material that accreted while still hot (1000-1200 K). Although the physical implausibility of hot accretion has been addressed [3], no comprehensive evaluation has been made of arguments in its favor. As shown below, these arguments are based on incomplete data, flawed experiments or improbable interpretations. Correlation between petrologic type and Ca in low-Ca pyroxene. Models of prograde metamorphism assume that, with increasing temperature, opx acquires Ca at the expense of diopside. Analyses of pyroxene in 10 H chondrites showed no correlation between Ca in pyroxene cores and increasing petrologic type [4], but more extensive data sets show such correlations [1,5,6]. A review of data for 51 OC [7] shows a progressive increase in the Wo content of low-Ca pyroxene with petrologic type: Wo 0.4-1.2 in type-3 and -4; Wo 1.2-1.6 in type-5; and Wo 1.6-2.2 in type-6. Striated opx. Undeformed striated opx were interpreted as having formed from inverted protopyroxene during slow cooling [8]; striated opx from H4 Quenggouk were found to convert into normal opx within 1 week during annealing at 1100 K [9]. Because prograde metamorphism probably lasted ~60 Ma [10], there should be no striated opx remaining in type-4 or -5 OC. However, samples of 99% twinned clinopyroxene (analogous to that in chondrules in type-3 OC) annealed for >3 weeks at <=1250 K exhibited only very minor inversion to opx [11-13]. These experiments are consistent with prograde metamorphism; it seems likely that Quenggouk pyroxene probably had a substantial proportion of opx lamellae to begin with. Spinodal decomposition textures and cooling rates. Spinodal decomposition textures in pyroxene in type 4-5 OC were observed to have the same periodicities as those in type-3 OC [14]; it was concluded that the textures must have formed during cooling after hot accretion. However, because spinodal decomposition textures develop over the temperature range 1400-1100 K [14,15] and type-4 and -5 OC were probably not heated above 1000 K and 1050 K, respectively [16], these textures are probably relicts of chondrule formation. It was also suggested [14] that compositional zoning in pyroxenes indicates that type-3 OC cooled more rapidly than type-4 to -5 OC. However, OC metallographic cooling rates are not correlated with petrologic type [17]. Furthermore, experimental data [13] show that rare thick opx lamellae in H4 Conquista could not have formed during single stage cooling as expected in autometamorphism; a two-stage cooling history involving rapid cooling during chondrule formation followed by parent-body annealing is more plausible. Polycrystalline taenite. Polycrystalline taenite in H/L3 Tieschitz was interpreted as a relict solidification structure that failed to anneal into monocrystalline taenite because of rapid cooling (1700 to 1000 K within days to weeks) [18]; by analogy, it was proposed that all H3-6 chondrites containing polycrystalline taenite cooled rapidly from 1700 K [4], an idea inconsistent with prograde metamorphism. However, cooling rates in equilibrated chondrites that were slow enough to permit significant growth of kamacite would erase prior solidification zoning in taenite by solid-state diffusion [19,20]. This hypothesis, confirmed by computer modeling [21], invalidates the assumption that equilibrated OC containing polycrystalline taenite cooled rapidly. Polycrystalline taenite is most likely a pre-metamorphic relict. Heterogeneous metal grains. Compositionally and texturally heterogeneous metal grains in L6 Bruderheim are unlikely to have survived solid-state diffusion during prograde metamorphism [22]; these authors favored hot accretion followed by low-temperature annealing. However, Bruderheim is a fragmental breccia of shock stage S4 [23] containing partly melted metal grains and opaque veins; heterogeneities in metallic Fe-Ni grains are due to post-metamorphic shock. Misshapen chondrules. A small proportion of chondrules in Tieschitz are non-spherical and seem to have molded themselves around one another while they were at least partly molten, possibly on the surface of a hot asteroid [24]. However, it is now clear that these conjoined objects are adhering or enveloping compound chondrules that fused in the nebula [25]; most are probably siblings that collided shortly after forming in the same heating event. Objects adjacent to the compound chondrules are separated by intervening matrix material; because matrix material is fine grained, porous, highly disequilibrated and unmelted [26,27], any complementarity in shape between adjacent objects and compound chondrules is either due to coincidence or jostling during chondrite compaction. Natural remanent magnetization (NRM). The orientations of the stable NRM in OC were found to be random at scales of ~1 mm3 [28]. Because metamorphic heating would erase the random magnetization, these authors opted for hot accretion. However, most OC appear to be fragmental breccias that contain scattered metal and silicate grains of aberrant compositions that were incorporated into their hosts after metamorphic equilibration [29,30]; by analogy to some CM chondrites which contain mm-size clasts that experienced different degrees of aqueous alteration [31], it is plausible that OC are also brecciated on mm-size scales. Such fine-scale brecciation could account for the random orientations of the stable NRM. References: [1] Dodd R. T. (1969) GCA, 33, 161-203. [2] McSween H. Y. et al. (1988) in Meteorites and the Early Solar System, 102-113, Univ. of Arizona, Tucson. [3] Haack H. et al. (1992) GRL, 19, 2235-2238. [4] Hutchison R. et al. (1980) Nature, 287, 787-790. [5] Keil K. and Fredriksson K. (1964) JGR, 69, 3487-3515. [6] Heyse J. V. (1978) EPSL, 40, 365-381. [7] Scott E. R. D. et al. (1986) Proc. LPSC 17th, in JGR, 91, E115-E123. [8] Ashworth J. R. (1980) EPSL, 46, 167-177. [9] Ashworth J. R. et al. (1984) Nature, 308, 259-261. [10] G"pel C. et al. (1994) EPSL, 121, 153-171. [11] Jones R. H. and Brearley A. J. (1988) Meteoritics, 23, 277. [12] Brearley A. J. and Jones R. H. (1988) Eos Trans. AGU, 69, 1506. [13] Brearley A. J. and Jones R. H. (1993) LPS XXIV, 185-186. [14] Watanabe S. et al. (1985) EPSL, 72, 87-98. [15] Robinson P. et al. (1977) Am. Mineral., 62, 857-873. [16] Dodd R. T. (1981) Meteorites: A Petrologic-Chemical Synthesis, Cambridge. [17] Taylor G. J. (1987) Icarus, 69, 1-13. [18] Bevan A. W. R. and Axon H. J. (1980) EPSL, 47, 353-360. [19] Scott E. R. D. and Rajan R. S. (1981) GCA, 45, 53-67. [20] Scott E. R. D. and Rajan R. S. (1981) GCA, 45, 1959. [21] Willis J. and Goldstein J. I. (1981) Nature, 293, 126-127. [22] Smith D. G. W. and Launspach S. (1991) EPSL, 102, 79-93. [23] St"ffler D. et al. (1991) GCA, 55, 3845-3867. [24] Hutchison R. et al. (1979) Nature, 280, 116-119. [25] Wasson J. T. et al. (1995) GCA, 59, 1847-1869. [26] Scott E. R. D. et al. (1984) GCA, 48, 1741-1757. [27] Nagahara H. (1984) GCA, 48, 2581-2595. [28] Morden S. J. and Collinson D. W. (1992) EPSL, 109, 185-204. [29] Scott E. R. D. et al. (1985) Proc. LPSC 16th, in JGR, 90, D137-D148. [30] Rubin A. E. (1990) GCA, 54, 1217-1232. [31] Rubin A. E. and Wasson J. T. (1986) GCA, 50, 307-315.
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