Abstract
The interstellar dust model of comets is used as a basis to simultaneously satisfy various observational constraints and to derive the porosity of comet dust. The observational constraints are: (1) the strengths of the 3.4 µm and 9.7 µm emission bands; (2) the shape of the 9.7 µm band; (3) the relative amount of silicates to organic materials; (4) the mass distribution of the dust. The method used involves precise calculation of the temperatures and emission characteristics of porous aggregates of interstellar dust as a function of their mass, porosity and distance to the sun and the wavelength. The results indicate a high porosity of comet dust in the range 0.93 < P < 0.98.
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Greenberg, J.M., Hage, J.I. (1991). From Interstellar Dust to Comets to Comet Dust: A Test of the Interstellar Dust Model of Comets. In: Greenberg, J.M., Pirronello, V. (eds) Chemistry in Space. NATO ASI Series, vol 323. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0695-2_14
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DOI: https://doi.org/10.1007/978-94-009-0695-2_14
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