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The porous structure of dust samples was observed by improving the SEM magnification.
The chemical structure of dust samples before and after explosion was analyzed by FTIR.
As previously noted, Hadamcik and Levasseur-Regourd (2003b) assumed a compact structure of dust particles in the haloes.
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The goal of this paper is to derive simplified formulae that explicitly indicate the dependence of dust ring formation on materials and structures of dust particles.
To reveal the effects of particle characteristics, including particle thermal characteristics and size distributions, on flame propagation mechanisms during dust explosions clearly, the flame structures of dust clouds formed by different materials and particle size distributions were recorded using an approach combining high-speed photography and a band-pass filter.
One more advantage of this model is that it is consistent with the data on comet dust composition obtained in situ for comet 1P/Halley and with the structure of Interplanetary Dust Particles (IDPs) (Jessberger et al., 2001).
The problem of the effect of the internal structure of the dust grains is more complicated.
If such an enhancement is observed, the enhanced flux reveals the inner structure of icy dust particles.
The motivation of this work was to show how a simple model (here: the coated sphere model) compare with the structure of complex dust particles.
To do this, our calculations only consider ices as the constituent (mainly CO); in the last section, we have included silicate in some aggregates in an attempt to study the influence of the internal structure of the dust grains.
However, despite the average in shapes and sizes tending to smooth the spectral substructure, if a doubled-peaked profile is observed in the range of 2138 2145 cm-1, it could be the consequence of the shape or internal structure of the dust grain (i.e., core-mantle particles or preponderance of certain shape), given the knowledge that core/mantles volume ratios also smooth out the multiple peaks.
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