Lunar dust characterization by polarimetric signature. I. Negative polarization branch of sphere aggregates of various porosities

Details Lunar dust characterization by polarimetric signature. I. Negative polarization branch of sphere aggregates of various porosities Lunar dust characterization by polarimetric signature. I. Negative polarization branch of sphere aggregates of various porosities

2008-03-25

arxiv.org/abs/0803.3617v1

Astronomy and Astrophysics

Astrophysics

7 pages, 8 figures, accepted for publication in Astronomy & Astrophysics

Scientific paper

10.1051/0004-6361:20079108

Context. In support of NASA's exploration program and the return to the Moon, the polarimetric signature of dispersed individual Lunar regolith dust grains is studied to enable the characterization of the dust exopsheric environment by remote, in-situ, and standoff sensing. Aims. We explore the value of the negative polarization branch (NPB) as a signature for characterizing individual grains to determine if it can be used in the same way as for surfaces of planets and atmosphereless bodies. Results. Calculations show that polarization phase curves for spherical grains exhibit a sharp transition over a narrow range of size parameter between two distinct regimes, one typical of Rayleigh scattering and another dominated by a large NPB. The linear polarimetric signature observed for aggregates is a composite of a) the polarization induced by individual grains composing the aggregate and b) the polarization due to the aggregate as a whole dust grain. The weight of each component varies depending on the porosity of the aggregate. An NPB similar to the one observed for atmosphereless astronomical bodies is present for different ranges of the size parameter depending on the value of the porosity. It appears as a remnant of the negative branch exhibited by the single spherical grains. The sharper, narrow negative branch that is measured for some granular surfaces in the laboratory or seen in astronomical observations is not observed here.

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