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• W143860690 abstract "Introduction: Micrometeorites are terrestrially collected extraterrestrial dust particles smaller than about a millimeter. The accretion rate, size distribution and composition of micrometeorites bears on numerous studies including: deducing the compositions of parent bodies; calibrating terrestrial sedimentation rates; interpreting the isotopic record of seawater; linking influx to global climate change; and assessing the role of ET materials in life processes. In 1995 Taylor et al. [1] retrieved ~ 200g of material from the bottom of the South Pole water well (SPWW) of which about 0.1% were cosmic spherules (melted micrometeorites). Using the particle size distribution, area suctioned and age of ice melted (1100–1500 AD) they computed a terrestrial accretion rate for cosmic spherules 50–700 μm in diameter of 1600 ± 300 tons/yr [1] or 4 ± 2 percent of the flux measured above the atmosphere [2]. We are repeating this analysis using samples collected in 2000 from the SPWW. Compared with 1995 collection, the 2000 samples have less iron-oxide contamination allowing us to find unmelted micrometeorites. We are analyzing the deployment dedicated to the central plateau. Because this area was vacuumed in 1995 the 2000 sample should contain only those particles derived from the older, 700– 1100 AD, ice [3] and allow us to calculate a flux for a second time period. We have found and mounted 3272 micrometeorites from the central plateau sample. We present a preliminary size distribution (as not all micrometeorites have yet been measured) and an estimate of unmelted to melted ratio for the different size fractions. Methods: The samples studied were collected in 2000 from the SPWW, a 4,000-m reservoir melting pre-industrial ice. The well’s central plateau was vacuumed and yielded ~ 10 g of material. We sieved this sample into >425, 250–425, 150– 250, 106–150 and 53–106μm size fractions. Using a binocular microscope we sorted 100% of the >150-μm fractions, 29% of the106-150 fraction and 9% of the 53–106μm fraction and removed all potential ET grains. We mounted and sectioned over 4000 particles. Using a SEM/EDAX we checked each particle for composition and found that 3272 of particles mounted were micrometeorites. Optical microscopy was used to size the particles and to classify them based on their cross-sectional textures. Results: The size distributions for the 1995 and for the 2000 plateau samples are shown in Figure 1. For the 2000 collection we show individual data points for micrometeorites >250μm, as these have all been sized, and plot the cumulative number of micrometeorites for the three smallest size fractions. The numbers of micrometeorites in the smallest two size fractions have been increased to account for the fact that only a portion of each size fraction was sorted. The best-fit line to the tail of the 2000 plateau sample has a slope of -4.5 slightly less steep than the -5.2 tail-slope calculated for the 1995 plateau sample [2]. Nevertheless the two curves are quite similar indicating that the size distributions from the two collections are similar. The 2000 collection has more micrometeorites than the 1995 collection. The addition of the unmelted component cannot explain the increased number as the unmelted micrometeorites would predominantly change the number of micrometeorites in the smaller size fractions. The fact that we found an order of magnitude more >250μm micrometeorites in the 2000 collection may be due to an increase in the plateau area as the well deepens or to an increase in the flux rate. Although we have not yet measured the plateau area our video records do not show an order of magnitude increase in the plateau area." @default.
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• W143860690 date "2007-01-01" @default.
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• W143860690 title "Size Distribution of Antarctic Micrometeorites" @default.
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