¹Dai, D., ^1,2Liu, S. ^1,2Liu, X.
Minerals 8, 240 Link to Article [DOI: 10.3390/min8060240]
¹Institute of Geology, Hunan University of Science and Technology, Xiangtan, China
²Hunan Provincial Key Laboratory of Shale Gas Resource Utilization, Xiangtan, China

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¹Kereszturi, A., ²Fintor, K.,³Gyollai, I., ⁴Kereszty, Z., ³Szabo, M., ^5,6Szalai, Z., ²Walter, H.
Geological Quarterly 62, 433-446 Link to Article [doi: 10.7306/gq.1416]
¹Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklos Astronomical Institute, Konkoly Thege Miklósút 15–17, Budapest, Hungary
²University of Szeged, Vulcano Petrology and Geochemistry Research Group, Department of Mineralogy, Geochemistry and Petrology, Hungary
³Research Centre for Astronomy and Earth Sciences, Institute for Geological and Geochemical Research, Hungary

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^1,2Xue, Y., ³Li, C.-H., ³Qi, Y., ^1,2Zhang, C., ^1,2Miao, B., ³Huang, F.
Acta Geochimica 37, 501-508 Link to Article [DOI
https://doi.org/10.1007/s11631-018-0279-2]
¹Institution of Meteorites and Planetary Materials Research, Guilin University of Technology, Guilin, China
²Key Laboratory of Planetary Geological Evolution at Universities of Guangxi Province, Guilin University of Technology, Guilin, China
³Key Laboratory of Crust-Mantle Materials and Environments, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China

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^1,2Feng Yin, ^3,4Zhiwei Liao, ^1,5Andrew Hursthouse, ²Deqiu Dai
Minerals 8, 139 Link to Article [https://doi.org/10.3390/min8040139]
¹Hunan Provincial Key Laboratory of Shale Gas Resource Utilization, Hunan University of Science and Technology, Xiangtan 411201, China
²Department of Geology, Hunan University of Science and Technology, Xiangtan 411201, China
³College of Resources and Environmental Science, Chongqing University, Chongqing 400044, China
⁴State Key Laboratory of Coal Mine Disaster Dynamics and Control, Chongqing University, Chongqing 400044, China
⁵School of Science and Sport, University of the West of Scotland, Paisley PA1 2BE, UK

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^1,2Kayama, M.,^3,4Nagaoka, ^5,6Niihara, T.
Minerals 8, 267 Link to Article [DOI: 10.3390/min8070267]
¹Creative Interdisciplinary Research Division, Frontier Research Institute for Interdisciplinary Sciences, Tohoku University, Sendai, Japan
²Department of Earth and Planetary Materials Science, Graduate School of Science, Tohoku University, Sendai, Japan
³Research Institute for Science and Engineering, Waseda University, Tokyo, Japan
⁴Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
⁵Department of Systems Innovation, University of Tokyo, Tokyo, Japan
⁶University Museum, University of Tokyo, Tokyo, Japan

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¹Britton, T.B., ²Goran, D., ¹Tong, V.S.
Materials Characterization 142, 422-431 Link to Article [https://doi.org/10.1016/j.matchar.2018.06.001]
¹Department of Materials, Imperial College London, United Kingdom
²Bruker Nano GmbH, Germany

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¹Juulia-Gabrielle Moreaua, ^1,2Tomas Kohout, ³KaiWünnemann
Physics of the Earth and Planetary Interiors 282, 25-38 Link to Article [https://doi.org/10.1016/j.pepi.2018.06.006]
¹Department of Geosciences and Geography, University of Helsinki, P.O. Box 64, FI-00014 Helsinki, Finland
²Institute of Geology, The Czech Academy of Sciences, Rozvojová 269, CZ-165 00 Prague 6 – Lysolaje, Czech Republic
³Museum für Naturkunde, Leibniz Institute for Evolution and Biodiversity Science, Invalidenstraße 43, 10115 Berlin, Germany

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¹Baziotis, I., ²Asimow, P.D., ²Hu, J., ³Ferrière, L., ²Ma, C., ⁴Cernok, A., ^4,5Anand, M., ³Topa, D.
Scientific Reports 8, 9851 Link to Article [DOI: 10.1038/s41598-018-28191-6]
¹Department of Natural Resources Management and Agricultural Engineering, Agricultural Univ. of Athens, Iera Odos 75, Athens, Greece
²California Institute of Technology, Division of Geological and Planetary Sciences, Pasadena, CA, United States
³Natural History Museum, Burgring 7, Vienna, Austria
⁴Planetary and Space Sciences, Open University, Milton Keynes, United Kingdom
⁵Department of Earth Sciences, Natural History Museum, London, United Kingdom

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¹Antoine S. G. Roth,¹Ingo Leya
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13186]
¹Institute of Physics, University of BernBern, Switzerland
Published by arrangement with John Wiley & Sons

Cosmogenic nuclides are useful for reconstructing the cosmic‐ray precompaction exposure history of the chondritic components in the early solar system. Here, we present He and Ne isotope data for 22 chondrules and 4 matrix samples from Miller Range (MIL) 090657, which is the third most pristine Renazzo‐type (CR) carbonaceous chondrite (CR2.7). The studied samples contain variable mixtures of galactic cosmic ray (GCR)‐produced cosmogenic noble gases and trapped noble gases of presolar origin. Remarkably, all chondrules and matrix samples have within analytical uncertainty almost identical nominal ²¹Ne cosmic‐ray exposure (CRE) ages in the range 3.45–6.20 Ma. The nominal ³He CRE ages are mostly discordant, possibly due to partial ³H and ³He losses and/or an inaccurate correction for trapped ³He. The absence of precompaction exposure effects longer than a few Ma in MIL 090657 is at variance with data for other CR chondrites. We conclude that most CR chondrules experienced the same precompaction exposure history—although the nature of the precompaction exposure differs between the chondrites—in regions of the disk that were either exposed to or shielded from GCRs but in which exposure effects due to solar wind and/or solar cosmic rays (SCRs) were negligible. The new data do not support the X‐wind model of Shu and coworkers.

^1,2Mingfang Liu, ^1,2Ai Du, ^1,2Tiemin Li, ^1,2Ting Zhang, ^1,2Zhihua Zhang, ³Guangwei Cao, ³Hongwei Li, ^1,2Jun Shen, ^1,2Bin Zhou
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2018.08.017]
¹Shanghai Key Laboratory of Special Artificial Microstructure Materials and Technology, Tongji University, Shanghai, 200092, P. R. China
²School of Physics Science and Engineering, Tongji University, Shanghai, 200092, P. R. China
³National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, P. R. China
Copyright Elsevier

As an attractive collector medium for hypervelocity particles, SiO2 aerogel has been deployed on outer space missions. Aiming at quantifying the complicated relationship between the penetration track and the residual grains, many attempts have been made on hypervelocity experiments and models. However, models were difficult to accord strictly well with experimental data attributed to many uncertainties including thermal effects, aerogel accretions and projectile ablation during the penetration. In this paper, impact experiments were conducted at various density silica aerogels (50∼120 kg•m−3) with regular soda-lime glass beads as projectiles. Varying degrees of thermal effects happened around and along track was observed by scanning electron microscopy. That energy distribution in the track released by hypervelocity projectile has a decreasing change. The regular data of the terminal A-β type track (the track with combined features) was found according to A-type tracks classification based on the conditions of vapor model (Domínguez, 2009). Just considering for projectile overcoming the crushing strength with uniform deceleration, the simple mechanism was confirmed by the data fitted well with the snowplow model (Domínguez et al., 2004). The result after tracks classification is due to the terminal track with few thermal effects and aerogel accretions. In addition, other two types of tracks formation processes were discussed.