Overview

Workshop: Silicates in Space

Silicates are one of the most abundant dust grains in circum- and interstellar environments. Detection of crystalline silicates has actively been reported since 1990 onwards due to the development of infrared (IR) telescope technologies. Although observational outcomes have provided diverse evidences and facts, the analysis of IR spectra obtained by observations is quite complex and difficult to deal with because physical and chemical properties play a decisive role in the shape and strength of the distinctive spectral features. For interpretation of observed spectra, both experimentally measured and simulated spectra have been applied. Silicate dust condensation experiments as well as model calculations have been carried out in order to deepen our understanding of the formation process of the most abundant silicate dust grains. Additionally, thanks to the advanced technologies, silicates in meteorites, IDPs, asteroid, and comets have been analyzed in the finest detail. However, formation and evolution processes of silicate dust grains have not been well understood yet such as how does silicate dust formation take place and how much silicates are formed? How does the phase transformation from crystalline to amorphous and vise verse take place? Does silicate formation start by surface growth on the high temperature condensates such as spinel and corundum or directly from a gas phase? Is dust grain formation possible under low temperatures like the ISM? How does silicate dust take a part in star and planet formation?

This workshop is for exchanging, gaining, and enlarging knowledge and information from participants' working in different fields in order to deepen mutual understanding with regards to silicate dust grains.