¹Pechersky,¹D.M., Markov, G.P.
Izvestiya, Physics of the Solid Earth 55, 287-297 Link to Article [DOI: 10.1134/S1069351319020083]
¹Schmidt Institute of Physics of the Earth, Russian Academy of Sciences (IPE RAS), Moscow, 123242, Russian Federation

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2F. Thiessen,^1,3A. A. Nemchin,^1,4J. F. Snape,^1,2M. J. Whitehouse
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13310]
¹Department of Geosciences, Swedish Museum of Natural History, SE‐104 05 Stockholm, Sweden
²Department of Geological Sciences, Stockholm University, SE‐106 91 Stockholm, Sweden
³Department of Applied Geology, Curtin University, Perth, WA, 6845 Australia
⁴Faculty of Earth and Life Sciences, VU Amsterdam, De Boelelaan 1085, 1081 HV Amsterdam, the Netherlands
Published by arrangement with John Wiley & Sons

U‐Pb ages of zircon in four different Apollo 14 breccias (14305, 14306, 14314, and 14321) were obtained by secondary ion mass spectrometry. Some of the analyzed grains occur as cogenetic, poikilitic zircon grains in lithic clasts, revealing magmatic events at ~4286 Ma, ~4200–4220 Ma, and ~4150 Ma. The age distribution of the crystal clasts in the breccias exhibits a minor peak at ~4210 Ma, which can be attributed to a magmatic event, as recorded in zircon grains located in noritic clasts. An age peak at ~4335 Ma is present in all four breccias, as well as zircon grains from different Apollo landing sites, enhancing the confidence that these grains recorded a global zircon‐forming event. The overall age distribution among the four breccias exhibits minor differences between the breccias collected farther away from the Cone Crater and the ones collected within the continuous ejecta blanket of the Cone Crater. A granular zircon grain yielded a ²⁰⁷Pb/²⁰⁶Pb age of 3936 ± 8 Ma, which is interpreted as an impact event. A similar age of 3941 ± 5 Ma (n = 17, MSWD = 0.89, P = 0.58) was obtained for a large zircon grain (~430 × 340 μm in size). This grain might have crystallized in the same impact melt sheet which formed the granular zircon or the age is representative of the final extrusion of KREEP magma. The majority of zircon grains, however, occur as isolated crystal clasts within the matrix and their ages cannot be correlated with any real events (impact or magmatic) nor can the possibility be excluded that these ages represent partial resetting of the U‐Pb system.

^1,2Makiko K. Haba,¹Jörn-Frederik Wotzlaw,^1,3Yi-Jen Lai,⁴Akira Yamaguchi,¹Maria Schönbächler
Nature Geoscience (in Press) Link to Article [DOI
https://doi.org/10.1038/s41561-019-0377-8]
¹ETH Zürich, Institute of Geochemistry and Petrology, Zürich, Switzerland
²Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo, Japan
³Macquarie GeoAnalytical, Department of Earth and Planetary Sciences, Macquarie University, Sydney, New South Wales, Australia
⁴National Institute of Polar Research, Tokyo, Japan

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Ninja Braukmüller,^1,2Frank Wombacher,^1,2Claudia Funk,^1,2Carsten Münker
Nature Geoscience (in Press) Link to Article [DOI
https://doi.org/10.1038/s41561-019-0375-x]
¹Institut für Geologie und Mineralogie, Universität zu Köln, Köln, Germany
²Steinmann Institut für Geologie, Mineralogie und Paläontologie, Universität Bonn, Poppelsdorfer Schloss, Bonn, Germany

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Cheng Zhu,^1,2Parker B. Crandall,³Jeffrey J. Gillis-Davis,³Hope A. Ishii,⁴John P. Bradley,³Laura M. Corley,¹Ralf I. Kaiser
Proceeding sof the National Academy of Sciences of the United States of America 116, 11165-11170 Link to Article [https://doi.org/10.1073/pnas.1819600116]
¹Department of Chemistry, University of Hawai‘i at Mānoa, Honolulu, HI 96822;bW. M. Keck Laboratory in Astrochemistry, University of Hawai‘i at Mānoa, Honolulu, HI 96822;
²W. M. Keck Laboratory in Astrochemistry, University of Hawai‘i at Mānoa, Honolulu, HI 96822;
³Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822

The source of water (H₂O) and hydroxyl radicals (OH), identified on the lunar surface, represents a fundamental, unsolved puzzle. The interaction of solar-wind protons with silicates and oxides has been proposed as a key mechanism, but laboratory experiments yield conflicting results that suggest that proton implantation alone is insufficient to generate and liberate water. Here, we demonstrate in laboratory simulation experiments combined with imaging studies that water can be efficiently generated and released through rapid energetic heating like micrometeorite impacts into anhydrous silicates implanted with solar-wind protons. These synergistic effects of solar-wind protons and micrometeorites liberate water at mineral temperatures from 10 to 300 K via vesicles, thus providing evidence of a key mechanism to synthesize water in silicates and advancing our understanding on the origin of water as detected on the Moon and other airless bodies in our solar system such as Mercury and asteroids.