^1,2M. K. McClure,¹C. Dominik,^3,4M. Kama
Astronomy & Astrophysics 642, L15 Link to Article [DOI https://doi.org/10.1051/0004-6361/202038912]
¹Anton Pannekoek Institute for Astronomy, Universiteit van Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands
²Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
³Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
⁴Tartu Observatory, University of Tartu, Observatooriumi 1, Tõravere 61602, Estonia

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¹M. Agúndez,²J. I. Martínez,²P. L. de Andres,¹J. Cernicharo,²J. A. Martín-Gago
Astronomy & Astrophysics 637, A59 Link to Article [DOI https://doi.org/10.1051/0004-6361/202037496]
¹Instituto de Física Fundamental, CSIC, C/ Serrano 123, 28006 Madrid, Spain
²Instituto de Ciencia de Materiales de Madrid, CSIC, C/ Sor Juana Inés de la Cruz 3, 28049 Cantoblanco, Spain

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¹T.Kohout et al. (>10)
Astronomy & Astrophysics 639, A146 Link to Article [DOI https://doi.org/10.1051/0004-6361/202037593]
¹Department of Geosciences and Geography, University of Helsinki, Finland
²Institute of Geology, The Czech Academy of Sciences, Czech Republic

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¹William Goode,¹Sascha Kempf,^2,3Jürgen Schmidt
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.pss.2021.105343]
¹LASP, University of Colorado, Boulder, CO, USA
²Institute of Geological Sciences, Freie Universität, Berlin, Germany
³Space Physics and Astronomy Research Unit, University of Oulu, Finland
Copyright Elsevier

Europa and Ganymede are both likely to have subsurface oceans (Carr et al., 1998; Khurana et al., 1998; Kivelson et al., 2000). Young surface features may provide an opportunity to sample material from either a subsurface ocean or bodies of liquid water near the surface (McCord et al., 1999, 2001). Detailed compositional information is of large interest for understanding the evolution, oceanic chemistry, and habitability of these moons. To develop an altitude-dependent model for the detectability of ejecta particle composition originating from surface features of a given size, we simulate detections by a dust analyzer with the capability of measuring compositional makeup on board a spacecraft performing close flybys of Europa and Ganymede (Postberg et al., 2011). We determine the origin of simulated detections of ejecta by backtracking their trajectories to the surface using velocity distributions given in the ejecta cloud model by Krivov et al. (2003). Our model is useful for designing flybys with typical closest approach altitudes, such as the ones planned for NASA’s Europa Clipper mission, where we wish to accurately identify the composition of surface features using a dust analyzer.</sup2,3<>

¹M.A.Barucci et al. (>10)
Astronomy & Astrophysics 637, L4 Link to Article [DOI https://doi.org/10.1051/0004-6361/202038144]
¹LESIA, Observatoire de Paris, Université PSL, CNRS, Université de Paris, Sorbonne Université, 92195 Principal Cedex Meudon, France

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¹W. F. Thi,^1,6S. Hocuk,²I. Kamp,^3,7P. Woitke,²Ch. Rab,⁴S. Cazaux,¹P. Caselli,^5,2M. D’Angelo
Astronomy & Astrophysics 635, A16 Link to Article [https://doi.org/10.1051/0004-6361/201731747]
¹Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85741 Garching, Germany
²Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
³SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK
⁴Faculty of Aerospace Engineering, Delft University of Technology, Delft, The Netherlands
⁵Zernike Institute for Advanced Materials, University of Groningen, PO Box 221, 9700 AE Groningen, The Netherlands
⁶CentERdata, Tilburg University, PO Box 90153, 5000 LE Tilburg, The Netherlands
⁷Centre for Exoplanet Science, University of St Andrews, St Andrews, UK

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¹Javier Cuadros,²Joseph R.Michalski,³Janice L.Bishop,¹Christian Mavris,⁴Saverio Fiore,⁵Vesselin Dekov
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2021.114704]
¹Department of Earth Sciences, Natural History Museum, Cromwell Road, London SW7 5BD, UK
²Department of Earth Sciences & Laboratory for Space Research, The University of Hong Kong, Hong Kong, China
³SETI Institute, Mountain View, CA 94043, USA
⁴Institute of Methodologies for Environmental Analysis, CNR, Department of Geoenvironmental and Earth Sciences, University of Bari, Via Orabona 4, 70125 Bari, Italy
⁵Department of Marine Resources and Energy, Tokyo University of Marine Science and Technology, 4-5-7 Konan, Minato-ku, Tokyo 108-8477, Japan
Copyright Elsevier

The cameras on the Pathfinder probe (Imager for Pathfinder) and the rovers Spirit and Opportunity (Panoramic Camera), Curiosity (Mast Camera) and Perseverance (Mast Camera-Z) produce visible-range spectra of limited wavelength resolution but of great target resolution which allows mineralogical analysis of selected areas within martian rocks. Laboratory spectra of relevant specimens were transformed into the spectra corresponding to each of the above cameras to increase our capability to interpret martian spectral data collected in-situ. The focus was on finding spectral features that can be detected by the cameras on Mars and are diagnostic of specific minerals. The samples are a collection of (1) Fe/Mg-phyllosilicates from submarine hydrothermal sites and (2) of rocks from acid alteration environments containing goethite, hematite, jarosite and Fe-bearing chlorite as these minerals are detectable in the extended visible range. Among all the samples, interstratified glauconite-nontronite has the most unique spectral features and should be easily detectable with the rover cameras. The spectral features of talc from Fe-bearing interstratified specimens are described. These data are especially relevant as glauconite and talc have been proposed to be fairly abundant on Mars and their detections are suggested from remote-sensing near-IR data. Several indices are proposed to assess Fe content on the investigated samples as well as mineral concentration of goethite and hematite. Among these indices, the normalized spectral slope in the range 420–600 nm increases with total Fe content for all samples, whether phyllosilicates, oxides or sulphates (R2 = 0.7–0.8). For pure phyllosilicates, the slope from 600 to 1010 nm decreases with increasing octahedral Fe (R2 = 0.75). An index for goethite produced excellent results assessing goethite concentration (R2 = 0.84). Of all cameras, Mast Camera reproduces the spectra with lowest fidelity and generates the poorest correlations between indices and tested variables. The other three cameras perform similarly.

¹Andrea Wenzel,²Justin Filiberto,³Natasha Stephen,⁴Susanne P. Schwenzer,⁵Samantha J. Hammond
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13737]
¹Department of Geology, Southern Illinois University, Carbondale, Illinois, 62901 USA
²Lunar and Planetary Institute, USRA, Houston, Texas, 77058 USA
³Plymouth Electron Microscopy Centre, University of Plymouth, Drake Circus, Plymouth, PL4 8AA UK
⁴AstrobiologyOU, School of Environment, Earth, and Ecosystems Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA UK
⁵School of Environment, Earth, and Ecosystems Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA UK
Published by arrangement with John Wiley & Sons

Northwest Africa 6963 (NWA 6963) is a coarse-grained, gabbroic Martian meteorite that further extends our Martian sample collection, both compositionally and texturally. Gabbroic shergottite NWA 6963 provides direct petrologic evidence of intrusive igneous conditions within the Martian crust. Here, we analyzed geochemical zoning profiles and microstructural-crystallographic information from electron backscattered diffraction of augite and pigeonite to constrain the crystallization history of NWA 6963. Compositional zoning profiles reveal pyroxenes with augite or pigeonite cores mantled by Fe-rich pigeonite rims. Our results suggest complex pyroxene textures and zoning profiles observed in pyroxenes in NWA 6963 are due to pyroxene accumulation from a crystallizing magma in a large intrusive environment (sill or magma chamber); however, without geologic context or companion samples, it is currently impossible to rule out accumulation at the base of a very large (>>100 m) differentiated flow.

¹C. Wöhler,¹A. Grumpe,²M. Bhatt,³A. A. Berezhnoy,³V. V. Shevchenko,²A. Bhardwaj
Astronomy & Astrophysics 630, L7 Link to Article [https://doi.org/10.1051/0004-6361/201935927]
¹Image Analysis Group, TU Dortmund University, Otto-Hahn-Str. 4, 44227 Dortmund, Germany
²Physical Research Laboratory, Ahmedabad 380009, India
³Sternberg Astronomical Institute, Moscow State University, Universitetskij Pr., 13, 119234 Moscow, Russia

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¹M.Ferus et al. (>10)
Astronomy & Astrophysics 630, A127 Link to Article [https://doi.org/10.1051/0004-6361/201935816]
¹J. Heyrovský Institute of Physical Chemistry, Czech Academy of Sciences, Dolejškova 3, 18223 Prague 8, Czech Republic

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