¹Calla O.P.N.,¹Sharma V.
Indian Journal of Radio and Space Physics 49, 59 – 78 Link to Article [ISSN 03678393]
¹International Centre for Radio Science, Khokariya Bera,Nayapura, Mandore, Jodhpur, 342 304, Rajasthan, India

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^1,2Bekaert, D.V. et al. (>10)
Science Advances 40, abg8329 Link to Article [DOI 10.1126/sciadv.abg8329]
¹NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, 02543, MA, United States
²Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, 02543, MA, United States

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¹Shiryaev A.A.,^2,6Trigub A.L.,³Voronina E.N.,^4,5,6Kvashnina K.O.,¹Bukhovets V.L.
Physical Chemistry Chemical Physics 23, 21729 – 21737 Link to Article [DOI 10.1039/d1cp02600c]
¹A.N. Frumkin Institute of Physical Chemistry and Electrochemistry Ras, Leninsky pr. 31 korp. 4, Moscow, 119071, Russian Federation
²National Research Center «kurchatov Institute», Moscow, Russian Federation
³Department of Physics, Lomonosov Moscow State University, Moscow, 119991, Russian Federation
⁴The Rossendorf Beamline at ESRF-The European Synchrotron CS40220, Grenoble Cedex 9, 38043, France
⁵Helmholtz Zentrum Dresden-Rossendorf (HZDR), Institute of Resource Ecology, PO Box 510119, Dresden, 01314, Germany
⁶Department of Chemistry, Lomonosov Moscow State University, Moscow, 119991, Russian Federation

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¹Chandran, S.R. et al. (>10)
Lithos 404-405, 106479 Link to Article [DOI 10.1016/j.lithos.2021.106479]
¹Department of Geology, University of Kerala, Thiruvananthapuram, 695581, India

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¹Masaaki Miyahara,²Naotaka Tomioka,³Luca Bindi
Progress in Earth and Planetary Science volume 8, Article number: 59 Link to Article [https://doi.org/10.1186/s40645-021-00451-6]
¹Graduate School of Advanced Science and Engineering, Hiroshima University, Higashihiroshima, 739-8526, Japan
²Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Nankoku, Kochi, 783-8502, Japan
³Dipartimento Di Scienze Della Terra, Università Degli Studi Di Firenze, Via G. La Pira 4, 50121, Florence, Italy

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¹Alexander N. Krot,²Michail I. Petaev,¹Kazuhide Nagashima
Progress in Earth and Planetary Science 8, 61 Link to Article [DOI https://doi.org/10.1186/s40645-021-00437-4]
¹Hawai’i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai’i at Mānoa, Honolulu, HI, 96822, USA
²Department of Earth and Planetary Sciences, Harvard University and Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, 02138, USA

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^1,2Kimur,^3,4Weisberg M.K.,²Takaki A.,^1,5Imae N.,^1,5Yamaguchi A.
Progress in Earth and Planetary Science 8, 55 Link to Article [DOI10.1186/s40645-021-00447-2]
¹National Institute of Polar Research, Tokyo, Japan
²Ibaraki University, Mito, Japan
³Kingsborough College and Graduate Center of the City University of New York, New York, United States
⁴American Museum of Natural History, New York, United States
⁵SOKENDAI, Tokyo, Japan

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¹Abdu Y.A.
Hyperfine Interactions 242, 5 Link to Article [DOI 10.1007/s10751-021-01729-3]
¹Department of Applied Physics and Astronomy, University of Sharjah, P.O. Box 27272, Sharjah, United Arab Emirates

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¹Hiroaki Kaneko,²Sota Arakawa,¹Taishi Nakamoto
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2021.114726]
¹Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8550, Japan
²Division of Science, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan
Copyright Elsevier

Coarse objects in chondrites such as chondrules and CAIs are mostly coated with fine-grained rims (FGRs). FGRs can be formed on the surface of free floating chondrules in a turbulent nebula, where dust aggregation also occurs. A former study has reported that the morphology of the dust populations accreting onto chondrules affects the initial structures of FGRs. It was revealed that, if monomer grains accrete onto chondrules, the smaller grains tend to accumulate near the surface of chondrules, and FGRs exhibit grain size coarsening from the bottom to the top. However, the study did not consider the effect of temporal growth of dust aggregates on FGRs formation. In this study, we calculate the aggregation of polydisperse monomer grains and their accretion onto chondrules. The following two different stages of dust aggregation can be identified: the monomer-aggregation stage and the BCCA-like stage. In the monomer-aggregation stage, monomer grains are incorporated into aggregates when the average aggregate size reaches the size of the monomer. In the BCCA-like stage, aggregates evolve fractally in a fashion similar to that of single size monomer grains. Based on the results of the previous study, we obtain the requisite conditions for chondrules to acquire monomer-accreting FGRs with grain size coarsening observed in some chondrites. In the case of similar size distribution as that of Inter Stellar Medium (ISM), the maximum grain size of m is widely () required for monomer accretion, while if turbulent intensity in a nebula is extremely weak (), a maximum grain size m is required. The monomer size distributions having larger mass fraction in the large grains compared to ISM might be necessary for the effective grain size coarsening.

¹Kenneth A. Farley,²Susan Taylor,¹Jonathan Treffkorn,²James H. Lever,²Anthony L. Gow
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13759]
¹California Institute of Technology, Pasadena, California, 91125 USA
²US Army Engineer Research and Development Center Cold Regions Research and Engineering Laboratory, Hanover, New Hampshire, 03755 USA
Published by arrangement with John Wiley & Sons

Researchers have characterized extraterrestrial (ET) helium, likely carried by interplanetary dust particles (IDPs), in deep-sea sediments spanning more than the last 100 Myr. Here we complement those low resolution and deep time studies by measuring He in modern Antarctic air and recent ice. We analyzed 180 air filter samples collected in 2017 and 2018 at the South Pole and detected 3He above blank levels in 178. The filters collected during the austral springs had elevated 3He in multiple subsamples indicating the presence of many individual IDPs and potentially, a temporal variation in the ET small particle flux. Our calculated mean 3He flux of 1.4 ± 1.2 × 10−12 cc STP cm−2 ka−1 is the first such measurement from air samples. We also melted, filtered, and analyzed one hundred and forty-one 1 m-long ice sections from a ˜2000-yr-old South Pole core. We detected 3He above blank levels in 139 of the 141 ice core samples and calculated an average flux of 1.2 ± 0.3 × 10−12 cc STP cm−2 ka−1. Our two flux values are within a factor of two of those calculated from stratospheric IDP concentrations, those previously measured for sections of the GISP2 and Vostok ice cores, and from sediment cores from different locations and ages. The similarity of these flux values over disparate time scales (1–108 yr) and geographic locations (90° S to equator) indicates modest temporal variability and remarkable agreement among diverse IDP archives. These data provide a compelling link from IDPs collected in the stratosphere to those recorded in deep time sedimentary archives.