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Paper: Interstellar Dust Models
Volume: 309, Astrophysics of Dust
Page: 691
Authors: Draine, B.T.
Abstract: Our knowledge of interstellar dust comes from various lines of evidence, mostly involving interaction of dust grains with electromagnetic radiation: interstellar extinction, polarization of starlight, scattering of starlight (reflection nebulae and the diffuse galactic light), scattering of X-rays, optical luminescence, and emission at infrared, far-infrared, submillimeter, and microwave frequencies. Additional "direct" evidence includes presolar interstellar grains preserved in meteorites and interstellar grains entering the solar system today. In addition, there are indirect lines of evidence, including interstellar depletions, formation of H2, and the inferred heating of gas by photoelectric emission. A viable dust model should satisfy all of these constraints. In addition, of course, the dust model should be consistent with general physical principles.

I will focus on one specific dust model — a mixture of carbonaceous particles and amorphous silicate particles (Weingartner & Draine 2001a, Li & Draine 2001) — and will compare this dust model to observational constraints.

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