¹K.Hadler,² D.J.P.Martin,³J.Carpenter,¹J.J.Cilliers,⁴A.Morse,¹S. Starr,¹J.N.Rasera,⁵K.Seweryn,³P.Reiss,³A.Meurisse
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104811]
¹Department of Earth Science and Engineering, Imperial College London, London, SW7 2AZ, UK
²European Space Agency ECSAT, Fermi Avenue, Harwell Campus, Didcot, Oxfordshire, OX11 0FD, UK
³European Space Agency ESTEC, Keplerlaan 1, 2201, AZ Noordwijk, the Netherlands
⁴School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
⁵Space Research Center of the Polish Academy of Sciences (CBK PAN), 18a Bartycka Str., 00-716, Warsaw, Poland

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¹P.Reiss,²F.Kerscher,³L.Grill
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2019.104795]
¹European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, the Netherlands
²Technical University of Munich, Institute for Energy Systems, Boltzmannstr. 15, 85748, Garching, Germany
³Technical University of Munich, Institute of Astronautics, Boltzmannstr. 15, 85748, Garching, Germany

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¹Zeman, J.,¹Ješkovský, M.,¹Kaizer, J.,²Pánik, J.,¹Kontuľ, I.,¹Staníček, J.,¹Povinec, P.P.
Journal of Radioanalytical and Nuclear Chemistry 322, 1897-1903 Link to Article [DOI: 10.1007/s10967-019-06851-9]
¹Faculty of Mathematics, Physics and Informatics, Centre for Nuclear and Accelerator Technologies (CENTA), Comenius University, Bratislava, 842 48, Slovakia
²Faculty of Medicine, Institute of Medical Physics, Biophysics, Informatics and Telemedicine, Comenius University, Bratislava, 813 72, Slovakia

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^1,2Ponomarev, D.S.,^1,2Litasov, K.D.,³Ishikawa, A.,¹Bazhan, I.S.,⁴Hirata, T.,¹Podgornykh, N.M.
Russian Geology and Geophysics 60, 752-767 Link to Article [DOI: 10.15372/RGG2019055]
¹V.S. Sobolev Institute of Geology and Mineralogy, Siberian Branch of the Russian Academy of Sciences, pr. Akademika Koptyuga 3, Novosibirsk, 630090, Russian Federation
²Novosibirsk State University, ul. Pirogova 2, Novosibirsk, 630090, Russian Federation
³Dept Earth Science and Astronomy, University of Tokyo, Komada, Meguro, Tokyo, 153-8902, Japan
⁴Geochemical Research Center, University of Tokyo, Hongo, Bunkyo, Tokyo, 113-8654, Japan

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¹Bogusz, P.,¹Gałązka-Friedman, J.,²Brzózka, K.,¹Jakubowska, M.,³Woźniak, M.,⁴Karwowski, Ł.,¹ Duda, P.
Hyperfine Interactions 240, 126 Link to Article [DOI: 10.1007/s10751-019-1659-7]
¹Faculty of Physics, Warsaw University of Technology, Koszykowa 75, Warsaw, 00-662, Poland
²Faculty of Mechanical Engineering, Department of Physics, University of Technology and Humanities, E. Stasieckiego 54, Radom, 26-600, Poland
³Faculty of Biology, University of Warsaw, Miecznikowa 1, Warszawa, 02-096, Poland
⁴Faculty of Natural Sciences, Institute of Earth Sciences, University of Silesia in Katowice, ul. Będzińska 60, Sosnowiec, 41-200, Poland

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¹Flynn, G.J.,²Durda, D.D.,³Molesky, M.J.,³May, B.A.,³Congram, S.N.,³Loftus, C.L., Reagan,³J.R.,³Strait, M.M.,⁴Macke, R.J.
International Journal of Impact Engineering 136, 103437 Link to Article [DOI: 10.1016/j.ijimpeng.2019.103437]
¹SUNY-Plattsburgh, 101 Broad St., Plattsburgh, NY 12901, United States
²Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, United States
³Alma College, Alma, MI 48801, United States
⁴Vatican Observatory, V-00120, Vatican City State

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¹Elsa Amsellem,^1,2Frédéric Moynier,^1,3Brandon Mahan,^2,4Pierre Beck
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2019.113593]
¹Université de Paris, Institut de physique du globe de Paris, CNRS, F-75005 Paris, France
²Institut Universitaire de France, Paris, France
³Department of Earth and Planetary Sciences, Macquarie University, Sydney, New South Wales 2109, Australia
⁴Institut de Planétologie et d’Astrophysique de Grenoble, Univ. Grenoble Alpes, CNRS, CNES, 38000 Grenoble, France
Copyright Elsevier

Carbonaceous chondrites are often considered potential contributors of water and other volatiles to terrestrial planets as most of them contain significant amounts of hydrous mineral phases. As such, carbonaceous chondrites are candidate building blocks for Earth, and elucidating their thermal histories is of direct importance for understanding the volatile element history of Earth and the terrestrial planets. A significant fraction of CM type carbonaceous chondrites are thermally metamorphosed or “heated” and have lost part of their water content. The origin and the timing of such heating events are still debated, as they could have occurred either in the first Myrs of the Solar System via short-lived radioactive heating, or later by impact induced heating and/or solar radiation. Since Rb is more volatile than Sr, and some heated CM chondrites are highly depleted in Rb, a dating system based on the radioactive decay of ⁸⁷Rb to ⁸⁷Sr (λ⁸⁷Rb = 1.393 × 10⁻¹¹ yr⁻¹) could be used to date the heating event relating to the fractionation of Rb and Sr. Here, we have leveraged the ⁸⁷Rb/⁸⁷Sr system to date the heating of five CM chondrites (PCA 02012, PCA 02010, PCA 91008, QUE 93005 and MIL 07675). We find that the heating events of all five meteorites occurred at least 3 Ga after the formation of the Solar System. Such timing excludes short-lived radioactive heating as the origin of thermal metamorphism in these meteorites, and relates such heating events to ages of collisional families of C-type asteroids.

¹Adrien Néri,²François Guyot,¹ Bruno Reynard,³Christophe Sotin
Earth and Planetary Science Letters 530, 115920 Link to Article [https://doi.org/10.1016/j.epsl.2019.115920]
¹University of Lyon, ENS de Lyon, CNRS, Lyon, France
²Museum National d’Histoire Naturelle, Sorbonne Université, IMPMC, UMR CNRS 7590, IRD UMR206, Paris, France
³Jet Propulsion Laboratory-California Institute of Technology, Pasadena, CA, USA
Copyright Elsevier

The inner structure of icy moons comprises ices, liquid water, a silicate rocky core and sometimes an inner metallic core depending on thermal evolution and differentiation. Mineralogy and density models for the silicate part of the icy satellites cores were assessed assuming a carbonaceous chondritic (CI) bulk composition and using a free-energy minimization code and experiments. Densities of other components, solid and liquid sulfides, carbonaceous matter, were evaluated from available equations of state. Model densities for silicates are larger than assessed from magnesian terrestrial minerals, by 200 to 600 kg.m⁻³ for the hydrated silicates, and 300 to 500 kg.m⁻³ for the dry silicates, due to the high iron bulk concentration in CI. The stability of Na-phlogopite in the silicate fraction up to 1300 K favors the trapping of most ⁴⁰K in the rocky/carbonaceous cores with important consequences for modeling of the thermal evolution of icy satellites. We find that CI density models of icy satellite cores taking into account only the silicate and metal/sulfide fraction cannot account for the observed densities and reduced moment of inertia of Titan and Ganymede without adding a lower density component. We propose that this low-density component is carbonaceous matter derived from insoluble organic matter, in proportion of ∼30-40% in volume and 15-20% in mass. This proportion is compatible with contributions from CI and comets, making these primitive bodies including their carbonaceous matter component likely precursors of icy moons, and potentially of most of the objects formed behind the snow line of the solar system.

^1,2T.Mannel et al. (>10)
Astronomy & Astrophysics 630, A26 Link to Article
[https://doi.org/10.1051/0004-6361/201834851]
¹Space Research Institute of the Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
²University of Graz, Universitätsplatz 3, 8010 Graz, Austria

¹Pavol Matlovič,¹Juraj Tóth,²Regina Rudawska,¹Leonard Kornoš,¹Adriana Pisarčíková
Astronomy & Astrophysics 629 A71 Link to Article
[https://doi.org/10.1051/0004-6361/201936093]
¹Faculty of Mathematics, Physics and Informatics, Comenius University, Bratislava, Slovakia
²ESTEC/ESA, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands

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