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Recent space missions have provided information on the physical and chemicalproperties of interstellar grains such as the ratio $\beta$ of radiationpressure to gravity acting on the grains in addition to the composition,structure, and size distribution of the grains. Numerical simulation on thetrajectories of interstellar grains captured by Stardust and returned to Earthconstrained the $\beta$ ratio for the Stardust samples of interstellar origin.However, recent accurate calculations of radiation pressure cross sections formodel dust grains have given conflicting stories in the $\beta$ ratio ofinterstellar grains. The $\beta$ ratio for model dust grains of so-called"astronomical silicate" in the femto-kilogram range lies below unity, inconflict with $\beta \sim 1$ for the Stardust interstellar grains. Here, Itackle this conundrum by re-evaluating the $\beta$ ratio of interstellar grainson the assumption that the grains are aggregated particles grown by coagulationand composed of amorphous MgSiO$_{3}$ with the inclusion of metallic iron. Mymodel is entirely consistent with the depletion and the correlation of majorrock-forming elements in the Local Interstellar Cloud surrounding the Sun andthe mineralogical identification of interstellar grains in the Stardust andCassini missions. I find that my model dust particles fulfill the constraintson the $\beta$ ratio derived from not only the Stardust mission but also theUlysses and Cassini missions. My results suggest that iron is not incorporatedinto silicates but exists as metal, contrary to the majority of interstellardust models available to date.

the astrophysical journal. letters

High Radiation Pressure on Interstellar Dust Computed by  Light-Scattering Simulation on Fluffy Agglomerates of Magnesium-silicate  Grains with Metallic-iron Inclusions