Variations in cometary dust composition from Giotto to Rosetta, clues to their formation mechanisms

Cécile Engrand 1 Jean Duprat 1 Emmanuel Dartois 2 Karim Benzerara 3 Hugues Leroux 4 Donia Baklouti 2 Anaïs Bardyn 5 Christelle Briois 5 Hervé Cottin 6 Henning Fischer 7 Nicolas Fray 6 Marie Godard 8 Martin Hilchenbach 7 Yves Langevin 2 John Paquette 7 Jouni Rynö 9 Rita Schulz 10 Johan Silén 9 Oliver Stenzel 7 Laurent Thirkell 5
1 CSNSM AS - Centre de Sciences Nucléaires et de Sciences de la Matière
2 IAS - Institut d'astrophysique spatiale
3 IMPMC - Institut de minéralogie, de physique des matériaux et de cosmochimie
4 UMET - Unité Matériaux et Transformations - UMR 8207
5 LPC2E - Laboratoire de Physique et Chimie de l'Environnement et de l'Espace
6 LISA (UMR_7583) - Laboratoire Interuniversitaire des Systèmes Atmosphériques
7 MPS - Max-Planck-Institut für Sonnensystemforschung
8 CSNSM - Centre de Sciences Nucléaires et de Sciences de la Matière
9 FMI - Finnish Meteorological Institute
10 ESA Scientific Support Office
Abstract : This paper reviews the current knowledge on the composition of cometary dust (ice, minerals and organics) in order to constrain their origin and formation mechanisms. Comets have been investigated by astronomical observations, space missions (Giotto to Rosetta), and by the analysis of cometary dust particles collected on Earth, chondritic porous interplanetary dust particles (CP-IDPs) and ultracarbonaceous Antarctic micrometeorites (UCAMMs). Most ices detected in the dense phases of the interstellar medium (ISM) have been identified in cometary volatiles. However, differences also suggest that cometary ices cannot be completely inherited from the ISM. Cometary minerals are dominated by crystalline Mg-rich silicates, Fe sulphides and glassy phases including GEMS (glass with embedded metals and sulphides). The crystalline nature and refractory composition of a significant fraction of the minerals in comets imply a high temperature formation/processing close to the proto-Sun, resetting a possible presolar signature of these phases. These minerals were further transported up to the external regions of the disc and incorporated in comet nuclei. Cometary matter contains a low abundance of isotopically anomalous minerals directly inherited from the presolar cloud. At least two different kinds of organic matter are found in dust of cometary origin, with low or high nitrogen content. N-poor organic matter is also observed in primitive interplanetary materials (like carbonaceous chondrites) and its origin is debated. The N-rich organic matter is only observed in CP-IDPs and UCAMMs and can be formed by Galactic cosmic ray irradiation of N2- and CH4-rich icy surface at large heliocentric distance beyond a ‘nitrogen snow line’.
Keywords : meteors meteorites extinction meteoroids comets: general minor planets asteroids: general interplanetary medium ISM: abundances dust
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CSNSM | CNRS | UNIV-ORLEANS | UNIV-PARIS7 | INRA | IMPMC | MNHN | ALLINSP | UPMC | UPEC-UPEM | IN2P3 | INSU | IRD | INC-CNRS | USPC | UNIV-PARIS-SACLAY | UNIV-LILLE | SORBONNE-UNIVERSITE | OSUC | LPC2E | PSL | OBSPM | SU-SCIENCES | UPEC | LISA

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Cécile Engrand, Jean Duprat, Emmanuel Dartois, Karim Benzerara, Hugues Leroux, et al.. Variations in cometary dust composition from Giotto to Rosetta, clues to their formation mechanisms. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2016, 464 (1), pp.S323-S330. ⟨10.1093/mnras/stw2844⟩. ⟨insu-01404154⟩

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