¹Suttle, M.D.,²Twegar, K.,³Nava, J.,³Spiess, R.,⁴Spratt, J.,^1,5Campanale, F.,¹ Folco, L.
Scientific Reports 9, 12426 Link to Article [DOI: 10.1038/s41598-019-48937-0]
¹Dipartimento di Scienze della Terra, Università di Pisa, Pisa, 56126, Italy
²Department of Chemistry, Istanbul Technological University, Istanbul, 34467, Turkey
³Dipartimento di Geoscienze, Via Gradenigo 6, Padova, 35131, Italy
⁴Department of Earth Science, The Natural History Museum, Cromwell Rd, South Kensington, London, SW7 5BD, United Kingdom
⁵Center for Nanotechnology Innovation@NEST, Istituto Italiano di Tecnologia (IIT), Piazza San Silvestro 12, Pisa, 56127, Italy

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

¹Liu, M.-C.,^2,3Han, J.,⁴Brearley, A.J.,¹Hertwig, A.T.
Science Advances 5, eaaw3350 Link to Article [DOI: 10.1126/sciadv.aaw3350]
¹Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, United States
²Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77058, United States
³NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX 77058, United States
⁴Department of Earth and Planetary Sciences, MSC03-2040, University of New Mexico, Albuquerque, NM 87131, United States

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¹J. Martin Laming,²Angelos Vourlidas,³Clarence Korendyke,³Damien Chua,⁴Steven R. Cranmer,¹Yuan-Kuen Ko,⁵Natsuha Kuroda,²Elena Provornikova,⁶John C. Raymond,²Nour-Eddine Raouafi
The Astrophysical Journal 879, 124 Link to Article [https://doi.org/10.3847/1538-4357/ab23f1]
¹Space Science Division, Code 7684, Naval Research Laboratory, Washington, DC 20375, USA
²Johns Hopkins University Applied Physics Laboratory, Laurel. MD 20723, USA
³Space Science Division, Code 7686, Naval Research Laboratory, Washington, DC 20375, USA
⁴Department of Astrophysical and Planetary Sciences, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309, USA
⁵University Corporation for Atmospheric Research (UCAR), Boulder, CO 80307, USA, and Space Science Division, Code 7684, Naval Research Laboratory, Washington DC 20375, USA
⁶Smithsonian Astrophysical Observatory, Cambridge, MA 02138, USA
⁷NRL/NRC Research Associate, Space Science Division, Code 7684, Naval Research Laboratory, Washington, DC 20375, USA
⁸Space Science Division, Code 7685, Naval Research Laboratory, Washington, DC 20375, USA

We examine the different element abundances exhibited by the closed loop solar corona and the slow speed solar wind. Both are subject to the first ionization potential (FIP) effect, the enhancement in coronal abundance of elements with FIP below 10 eV (e.g., Mg, Si, Fe) with respect to high-FIP elements (e.g., O, Ne, Ar), but with subtle differences. Intermediate elements, S, P, and C, with FIP just above 10 eV, behave as high-FIP elements in closed loops, but are fractionated more like low-FIP elements in the solar wind. On the basis of FIP fractionation by the ponderomotive force in the chromosphere, we discuss fractionation scenarios where this difference might originate. Fractionation low in the chromosphere where hydrogen is neutral enhances the S, P, and C abundances. This arises with nonresonant waves, which are ubiquitous in open field regions, and is also stronger with torsional Alfvén waves, as opposed to shear (i.e., planar) waves. We discuss the bearing these findings have on models of interchange reconnection as the source of the slow speed solar wind. The outflowing solar wind must ultimately be a mixture of the plasma in the originally open and closed fields, and the proportions and degree of mixing should depend on details of the reconnection process. We also describe novel diagnostics in ultraviolet and extreme ultraviolet spectroscopy now available with these new insights, with the prospect of investigating slow speed solar wind origins and the contribution of interchange reconnection by remote sensing.

^1,2,3Daly, L.,¹Lee, M.R.,⁴Piazolo, S.,¹Griffin, S.,⁵Bazargan, M.,^1,6Campanale, F.,¹ Chung, P.,¹Cohen, B.E.,¹Pickersgill, A.E.,¹Hallis, L.J.,⁷Trimby, P.W.,⁸Baumgartner, R.,² Forman, L.V.,^9,10Benedix, G.K.
Science Advances 5, eaaw5549 Link to Article [DOI: 10.1126/sciadv.aaw5549]
¹School of Geographical and Earth Sciences, University of Glasgow, Glasgow, G12 8QQ, United Kingdom
²Space Science and Technology Centre, School of Earth and Planetary Sciences, Curtin University, GPO Box U1987, Perth, WA 6845, Australia
³Australian Centre for Microscopy and Microanalysis, University of Sydney, NSW 2006, Australia
⁴School of Earth and Environment, University of Leeds, Leeds, LS2 9JT, United Kingdom
⁵Department of Earth Sciences, Uppsala University, Uppsala, Sweden
⁶Dipartimento di Scienze della Terra, Università di Pisa ,via Santa Maria 53, Pisa, 56126, Italy
⁷Oxford Instruments Nanoanalysis, High Wycombe, HP12 3SE, United Kingdom
⁸Australian Centre for Astrobiology, University of New South Wales, Sydney, NSW 2052, Australia
⁹Department of Earth and Planetary Sciences, Western Australia Museum, Locked Bag 49, Welshpool, WA 6986, Australia
¹⁰Planetary Science Institute, Suite 106, 1700 East Fort Lowell, Tucson, United States

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^1,2Charles C. Monson,³Dustin Sweet,³Branimir Segvic,³Giovanni Zanoni,²Kyle Balling,^2,4Jacalyn M. Wittmer,⁵G. Robert Ganis,⁶Guo Cheng
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13401]
¹Illinois State Geological Survey, University of lllinois at Urbana-Champaign, 615 East Peabody Drive, Champaign, Illinois
61820, USA
²Department or Geology, University of Illinois at Urbana-Champaign, 1301 West Green Street, Urbana, lllinois 61801, USA
³Department of Geosciences, Texas Tech University, 1200 Memorial Circle, Lubbock, Texas 79409, USA
⁴Department of Geological Sciences, State University of New York at Geneseo, 1 College Circle, Geneseo, New York
14454, USA
⁵Consulting Geologist, 749 Burlwood Drive, Southcrn Pincs. North Carolina 28387, USA
⁶Department of Earth and Environmental Sciences, 115 Trowbridge Hall, Jowa City, Iowa 52242, USA
Published by arrangement with John Wiley & Sons

The Glasford structure in Illinois (USA) was recognized as a buried impact craterin the early 1960s but has never been reassessed in light of recent advances in planetaryscience. Here, we document shatter cones and previously unknown quartz microdeformationfeatures that support an impact origin for the Glasford structure. We identify the 4 kmwide structure as a complex buried impact crater and describe syn- and postimpact depositsfrom its annular trough. We have informally designated these deposits as the KingstonMines unit (KM). The fossils and sedimentology of the KM indicate a marine depositionalsetting. The various intervals within the KM constitute a succession of breccia, carbonate,sandstone, and shale similar to marine sedimentary successions preserved in other craters.Graptolite specimens retrieved from the KM place the time of deposition at approximately4552 Ma (Late Ordovician, Sandbian). This age determination suggests a possible linkbetween the Glasford impact and the Ordovician meteorite shower, an increase in the rateof terrestrial meteorite impacts attributed to the breakup of the L-chondrite parent body inthe main asteroid belt.