Light scattering by fluffy Mg–Fe–SiO and C mixtures as cometary analogs (PROGRA 2 experiment)

• Published in: Icarus (New York, N.Y. 1962) Vol. 190; no. 2; pp. 660 - 671
• Main Authors: Hadamcik, E., Renard, J.-B., Rietmeijer, F.J.M., Levasseur-Regourd, A.C., Hill, H.G.M., Karner, J.M., Nuth, J.A.
• Format: Journal Article
• Language: English
• Published: San Diego, CA Elsevier Inc 01.10.2007; Elsevier
• Subjects: Astronomy; Atmospheric and Oceanic Physics; Comets; dust; Earth, ocean, space; Exact sciences and technology; Mineralogy; Physics; Polarimetry; Solar system; Comets; Mineralogy; Polarimetry; Grain size; Particle size; Light scattering; dust; Mineralogy; Polarimetry; Physical properties; Scattered light; Physical parameter; Cometary coma; Linear polarization; Solar system; dust
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2007.03.010

Cometary particles mainly consist of silicates and carbon compounds; they seem to be fluffy aggregates of tiny grains, as found in some IDPs. The linear polarization of the scattered light is an efficient method to characterize their physical properties. Laboratory simulations of light scattering by cometary analog particles help to disentangle different physical parameters by comparison with observational data. We present here polarization laboratory results with nine samples levitating particles: five samples of vapor-condensed magnesiosilica, one ferrosilica smoke, a mixture of magnesio–ferrosilica smokes, one mixture of ferrosilica with carbon and one mixture of magnesio–ferrosilica with carbon. The phase curves are bell-shaped with a maximum polarization at a phase range of (80°–100°). A shallow negative branch can be present at phase angles smaller than 20°. The different characteristics of the phase curves are discussed considering the size and the structure of the constituent grains and the size of the particles. For the five magnesiosilica samples, the maximum in polarization is in the 40% range (close to cometary values), and no wavelength dependence is detected; the negative branch, whose presence seems to be linked to the presence of large aggregates of fine silica (SiO 2) grains, does not always exist. For the ferrosilica smoke, the maximum in polarization is about 30% in red light (632.8 nm) and 40% in green light (543.5 nm); the negative branch occurs for phase angles smaller than 20°. For the two mixtures with carbon black, the polarization spectral gradient is positive, as expected for cometary analog particles. Finally, the phase curves obtained for agglomerates of magnesio–ferrosilica and carbon (expected to be the main components of cometary particles) are comparable to those obtained by remote observations of dust in cometary comae.