High Radiation Pressure on Interstellar Dust Computed by
  Light-Scattering Simulation on Fluffy Agglomerates of Magnesium-silicate
  Grains with Metallic-iron Inclusions
  Recent space missions have provided information on the physical and chemical
properties of interstellar grains such as the ratio $\beta$ of radiation
pressure to gravity acting on the grains in addition to the composition,
structure, and size distribution of the grains. Numerical simulation on the
trajectories of interstellar grains captured by Stardust and returned to Earth
constrained the $\beta$ ratio for the Stardust samples of interstellar origin.
However, recent accurate calculations of radiation pressure cross sections for
model dust grains have given conflicting stories in the $\beta$ ratio of
interstellar grains. The $\beta$ ratio for model dust grains of so-called
"astronomical silicate" in the femto-kilogram range lies below unity, in
conflict with $\beta \sim 1$ for the Stardust interstellar grains. Here, I
tackle this conundrum by re-evaluating the $\beta$ ratio of interstellar grains
on the assumption that the grains are aggregated particles grown by coagulation
and composed of amorphous MgSiO$_{3}$ with the inclusion of metallic iron. My
model is entirely consistent with the depletion and the correlation of major
rock-forming elements in the Local Interstellar Cloud surrounding the Sun and
the mineralogical identification of interstellar grains in the Stardust and
Cassini missions. I find that my model dust particles fulfill the constraints
on the $\beta$ ratio derived from not only the Stardust mission but also the
Ulysses and Cassini missions. My results suggest that iron is not incorporated
into silicates but exists as metal, contrary to the majority of interstellar
dust models available to date.
