Size Frequency Distributions of Fluid Drop Chondrules in Ordinary Chondrites

King, Trude V.V.; King, E. A.

doi:10.1111/j.1945-5100.1979.tb00482.x

Cited by 46 publications

(30 citation statements)

References 9 publications

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“…Crystalline lunar spherules are as abundant in the present Ap-0110 14 breccias as chondrules are in certain chondrite classes such as the CM chondrites that are -5 vol% chondrules. They also have very similar cumulative size-frequency distributions to many meteorite chondrule populations, which might suggest a similar mode of formation (see King and King, 1979;Rubin and Grossman, 1987;Rubin, 1989).…”

Section: Discussionmentioning

confidence: 75%

The crystalline lunar spherules: Their formation and implications for the origin of meteoritic chondrules

Symes

Sears

Akridge

et al. 1998

Meteorit & Planetary Scien

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Abstract-Crystalline lunar spherules (CLS) from three thin sections of Apollo 14 regolith breccias (143 18,6; 14318,48 and 14315,20) have been examined. The objects have been classified and their abundances, size distributions, bulk compositions, and (where possible) plagioclase compositions determined. By number, 64% consist predominantly of very tine-grained equant plagioclase grains but can also contain larger (-50 pm) feldspar crystals (type X), while 22% contain plagioclase lathes in a fine-grained mafic mesostasis (type Y ) . Plagioclase in both spherule types displays bright yellow cathodoluminescence that is conspicuous among the blue CL of the normal feldspar of the breccias. Type Z spherules (5%) contain feldspar with blue CL and minor amounts of olivine and pyroxene. Type Q spherules (4%) contain feldspar with yellow CL but in a luminescent mesostasis (of quartz or feldspar?). A few spherules are mixtures of type Y and type X textures. Most type X spherules, and a few type Y spherules, have fine-grained opaque rims. Compound objects were also found and consist of two or more CLS that appear to have collided while still plastic or molten. The CLS are thought to be impact spherules that crystallized in free flight, their coarse textures suggesting fairly slow cooling rates (-< 1 "Us). The abundance of the CLS resembles that of chondrules in the CM chondrite Murchison, and their cumulative size-frequency distributions are very similar to those of the chondrules in several meteorite classes. The bulk compositions of the CLS do not resemble regoliths at any of the Apollo sites, including Apollo 14, or any of the common impact glasses, but they do resemble the bulk compositions of several lunar meteorites and the impact glasses they contain. The Apollo 14 site is located on a region containing Imbrium ejecta, and we suggest that the CLS derive from the Imbrium impact. Ballistic calculations indicate that only impact events of this size on the Moon are capable of producing melt spherules with the required free flight times and slow cooling rates. Smaller impacts produce glassy spherules and agglutinates. As has been pointed out many times, the CLS have many properties in common with meteoritic chondrules. While much remains unclear, difficulties with a nebular origin and new developments in chondrule chronology, studies of asteroid surfaces and impact ejecta behavior, and the present observations indicate that meteoritic chondrules could have formed by impact.

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Section: Discussionmentioning

confidence: 75%

The crystalline lunar spherules: Their formation and implications for the origin of meteoritic chondrules

Symes

Sears

Akridge

et al. 1998

Meteorit & Planetary Scien

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“…Grossman et al (1988a) reviewed both the physical, textural, and chemical properties of chondrules. They cited the data of Rubin and Keil (1984 and unpublished data) and King and King (1979) to arrive at their assessment that the mean L chondrite chondrule diameter lies between 600 and 800 m. Weisberg et al (2006) cited 700 m from the Grossman et al (1988a) work as a mean chondrule diameter. Rubin (2000Rubin ( , 2005 cited Grossman et al (1988a) but quoted a mean apparent diameter of 500 m. Later, Rubin (2010) quoted 400 m as an estimate for an L chondrite chondrule mean diameter.…”

Section: Chondritesmentioning

confidence: 96%

“…The 132 chondrules from Khohar (L3.6) were found to have a median apparent diameter of 620 m ( Table 2). The 58 chondrules from Mezö-Madaras (L3.7) were found to have a median apparent diameter of 490 m. As with the H chondrites, King and King (1979) reported their data using the statistical parameters commonly used in sedimentology, and we summarize available data in Table 2. Ikeda and Takeda (1979) (Table 2).…”

Section: Chondritesmentioning

confidence: 98%

Chondrule size and related physical properties: A compilation and evaluation of current data across all meteorite groups

et al. 2015

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“…(King and King (1979) measured apparent diameters of 45 chondrules from a single LL chondrite (Parnallee, LL3.7). Gooding (1979) measured the true sizes of a total of 46 chondrules separated from three EL chonhites (Chainpur, LL3.4; Semarkona, LL3.0; Ngawi, LE3.6), but his separation technique excluded all LL3 chondrules with diameters smaller than 510 pm.…”

Section: Chondrulesmentioning

confidence: 99%

Size‐frequency distributions of chondrules and chondrule fragments in LL3 chondrites: Implications for parent‐body fragmentation of chondrules

Nelson

Rubin

2002

Meteorit & Planetary Scien

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Abstract-We measured the sizes and textural types of 719 intact chondrules and 1322 chondrule fragments in thin sections of Semarkona (LL3.0), Bishunpur (LL3. l), Krymka (LL3. I), Piancaldoli (LL3.4) and Lewis Cliff 88175 (LL3.8). The mean apparent diameter of chondrules in these LL3 chondrites is 0.80 q5 units or 570 pm, much smaller than the previous rough estimate of -900 pm. Chondrule fragments in the five LL3 chondrites have a mean apparent cross-section of 1.60 q5 units or 330 pm. The smallest fi-agments are isolated olivine and pyroxene grains; these are probably phenocrysts liberated from disrupted porphyritic chondrules. All five LL3 chondrites have fragment1 chondrule number ratios exceeding unity, suggesting that substantial numbers of the chondrules in these rocks were shattered. Most fragmentation probably occurred on the parent asteroid. Porphyritic chondrules (porphyritic olivine + porphyritic pyroxene + porphyritic olivine-pyroxene) are more readily broken than droplet chondrules (barred olivine + radial pyroxene + cryptocrystalline). The porphyritic fragmentkhondrule number ratio (2.0) appreciably exceeds that of droplet-textured objects (0.9). Intact droplet chondrules have a larger mean size than intact porphyritic chondrules, implying that large porphyritic chondrules are fragmented preferentially. This is consistent with the relatively low percentage of porphyritic chondrules within the set of the largest chondrules (57%) compared to that within the set of the smallest chondrules (81%). Differences in mean size among chondrule textural types may be due mainly to parent-body chondrule-fragmentation events and not to chondruleformation processes in the solar nebula.

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Size Frequency Distributions of Fluid Drop Chondrules in Ordinary Chondrites

Abstract: The size frequency distributions of fluid drop chondrules in 11 ordinary chondrites (five H3, one H4, four L3, one LL3)

Cited by 46 publications

References 9 publications

The crystalline lunar spherules: Their formation and implications for the origin of meteoritic chondrules

The crystalline lunar spherules: Their formation and implications for the origin of meteoritic chondrules

Chondrule size and related physical properties: A compilation and evaluation of current data across all meteorite groups

Size‐frequency distributions of chondrules and chondrule fragments in LL3 chondrites: Implications for parent‐body fragmentation of chondrules

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