Physical properties of dust in the solar system : relevance of a computational approach and of measurements under microgravity conditions

Details Physical properties of dust in the solar system : relevance of a computational approach and of measurements under microgravity conditions Physical properties of dust in the solar system : relevance of a computational approach and of measurements under microgravity conditions

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..20.1585l&link_type=abstract

Advances in Space Research, Volume 20, Issue 8, p. 1585-1594.

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Dust agglomerates/particles in the solar system (e.g. regoliths, cometary comae, interplanetary dust) are irregular aggregates whose scattering properties (phase functions of the intensity and polarization of scattered light) are drastically different from those of Mie spheres. However, the observation of the light they scatter may provide information on their physical properties. If the mechanism which makes up the aggregates is invariant with time, they are likely to be fractal particles, i.e. clusters formed of individual monomers. Computations have been made using a Discrete Dipole Approximation with hundreds of monomers; comparison with the observations suggests that regoliths or dust clouds have a fractal dimension of the order of 2, and consist of fluffy particles formed by Ballistic Cluster-Cluster aggregation. To built the reference database required for deriving the physical properties of these fluffy dust aggregates, and to avoid any modification of the particles properties by levitation techniques, it has been suggested to measure the scattering properties of numerous samples under microgravity conditions. Results obtained during parabolic flights show some discrepancy at large phase angles between the results obtained under Earth's gravity and microgravity conditions, the latter being more reminiscent of solar system observations.

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