^1,2M. Marsset, ²P. Vernazza, ^3,4M. Birlan, ⁵F. DeMeo, ⁵R. P. Binzel, ¹C. Dumas, ¹J. Milli, ^3,4M. Popescu4,3
¹European Southern Observatory (ESO), Alonso de Córdova 3107, 1900 Casilla Vitacura, Santiago, Chile
²Aix Marseille University, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
³IMCCE, Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France
⁴Astronomical Institute of the Romanian Academy, 5 Cuţitul de Argint, 040557 Bucharest, Romania
⁵Department of Earth, Atmospheric and Planetary Sciences, MIT, 77 Massachusetts Avenue, Cambridge, MA, 02139, USA

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Reference
Marsset M, Vernazza P, Birlan M, DeMeo F, Binzel RP, Dumas C, Milli J, Popescu M (2016) Compositional characterisation of the Themis family. Astronomy & Astrophysics 586 A15
Link to Article [http://dx.doi.org/10.1051/0004-6361/201526962]

¹C. Tubiana, ^1,2C. Snodgrass, ³R. Michelsen, ³H. Haack, ¹H. Böhnhardt, ⁴A. Fitzsimmons, ⁵I. P. Williams
¹Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 33077 Göttingen, Germany
²Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, UK
³Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, 1350 Copenhagen, Denmark
⁴Astrophysics Research Centre, Department of Physics and Astronomy, Queen’s University Belfast, Belfast BT7 1NN, UK
⁵School of Physics and Astronomy, Queen Mary, University of London, London E1 4NS, UK

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Reference
Tubiana C, Snodgrass C, Michelsen R, Haack H, Böhnhardt H, Fitzsimmons A, Williams IP (2016) 2P/Encke, the Taurid complex NEOs and the Maribo and Sutter’s Mill meteorites. Astronomy & Astrophysics 584, A97
Link to Article [http://dx.doi.org/10.1051/0004-6361/201425512]

¹M. Hilchenbach (>10)*
¹Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, D-37077 Göttingen, Germany
*Find the extensive, full author and affiliation list on the publishers website

The COmetary Secondary Ion Mass Analyser instrument on board ESA’s Rosetta mission has collected dust particles in the coma of comet 67P/Churyumov–Gerasimenko. During the early-orbit phase of the Rosetta mission, particles and particle agglomerates have been imaged and analyzed in the inner coma at distances between 100 km and 10 km off the cometary nucleus and at more than 3 AU from the Sun. We identified 585 particles of more than 14 μm in size. The particles are collected at low impact speeds and constitute a sample of the dust particles in the inner coma impacting and fragmenting on the targets. The sizes of the particles range from 14 μm up to sub-millimeter sizes and the differential dust flux size distribution is fitted with a power law exponent of −3.1. After impact, the larger particles tend to stick together, spread out or consist of single or a group of clumps, and the flocculent morphology of the fragmented particles is revealed. The elemental composition of the dust particles is heterogeneous and the particles could contain typical silicates like olivine and pyroxenes, as well as iron sulfides. The sodium to iron elemental ratio is enriched with regard to abundances in CI carbonaceous chondrites by a factor from ~1.5 to ~15. No clear evidence for organic matter has been identified. The composition and morphology of the collected dust particles appear to be similar to that of interplanetary dust particles.

Reference
Hilchenbach M et al. (2016) COMET 67P/CHURYUMOV–GERASIMENKO: CLOSE-UP ON DUST PARTICLE FRAGMENTS. The Astrophysical Journal (Letters) 816, L32
Link to Article [http://dx.doi.org/10.3847/2041-8205/816/2/L32http://dx.doi.org/10.3847/2041-8205/816/2/L32]