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This review focuses on numerical approaches to deducing the light-scatteringand thermal-emission properties of primitive dust particles in planetarysystems from astronomical observations. The particles are agglomerates of smallgrains with sizes comparable to visible wavelength and compositions beingmainly magnesium-rich silicates, iron-bearing metals, and organic refractorymaterials in pristine phases. These unique characteristics of primitive dustparticles reflect their formation and evolution around main-sequence stars ofessentially solar composition. The development of light-scattering theories hasbeen offering powerful tools to make a thorough investigation of lightscattering and thermal emission by primitive dust agglomerates in such acircumstellar environment. In particular, the discrete dipole approximation,the T-matrix method, and effective medium approximations are the most populartechniques for practical use in astronomy. Numerical simulations of lightscattering and thermal emission by dust agglomerates of submicrometer-sizedconstituent grains have a great potential to provide new state-of-the-artknowledge of primitive dust particles in planetary systems. What is essentialto this end is to combine the simulations with comprehensive collections ofrelevant results from not only astronomical observations, but also in-situ dataanalyses, laboratory sample analyses, laboratory analogue experiments, andtheoretical studies on the origin and evolution of the particles.

Light Scattering and Thermal Emission by Primitive Dust Particles in Planetary Systems