FROM INTERSTELLAR DUST TO COMETS - A UNIFICATION OF OBSERVATIONAL CONSTRAINTS

The interstellar dust model of comets is numerically worked out to satisfy simultaneously several basic constraints provided by observations of comet Halley, and to derive the porosity of coma dust. The observational constraints are (1) the strengths of the 3.4 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 calculations 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 that coma dust has a porosity in the range 0.93 < P < 0.975, i.e., a packing factor of 0.07 or less, consistent with independent observations of comet densities of 0.6 g cm-3 > ρc > 0.26 g cm-3 and meteor densities of less than 0.2 g cm-3.