Structure of Cometary and Interplanetary Dust, a Clue to the Formation and Early Evolution of Dust Particles in the Solar System

Astronomy and Astrophysics – Astronomy

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Cometary dust particles have been suspected to be fragile since the Giotto and Vega missions to comet Halley. More recently, numerous observations of the solar light scattered by dust particles in comet Hale-Bopp coma, together with versatile numerical simulations, have allowed us to suggest that these particles are likely to be built of both very fluffy aggregates and of more compact grains, with (to the first order) equivalent proportions in mass of absorbing material and transparent silicates [1,2]. The same approach, used to fit zodiacal light observations, indicates that a significant proportion of fluffy absorbing particles is found in the interplanetary dust cloud [3]. Laboratory simulations also lead to similar results, with e.g. polarimetric phase curves obtained for agglomerates of magnesio-ferrosilica comparable to those observed for cometary dust [4]. These estimations are now confirmed by the analysis of Stardust samples, with, e.g. evidence for both dense grains and aggregates with low bulk density within the coma of comet Wild 2 [5]. The relevance of such a structure for the formation and early evolution of dust particles in the solar system will be discussed.
[1] Lasue & Levasseur-Regourd, JQSRT 100, 220-236, 2006.
[2] Levasseur-Regourd, Mukai, Lasue, Okada, PSS, 55, 1010-1020, 2007.
[3] Lasue, Levasseur-Regourd, Fray, Cottin, A&A, in press, 2007
[4] Hadamcik, Renard, Rietmeijer, Levasseur-Regourd et al., Icarus, in press, 2007
[5] Hoerz, Bastien, Borg, Bradley et al., Science 314, 1716 - 1719, 2006

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