By studying the origins of this dust, we can know more about it. By studying the dust at its origins near stars, we may learn more about its characteristics in interstellar space. All stars have some sort of stellar wind where material from their surfaces is ejected outward driven by radiative pressure. In late-type giant stars, typically larger and cooler than the sun, this wind can contain many particles, not just hydrogen, but heavier elements as well. As material leaves the surface, two forces act upon it.
Radiation pressure pushes the material outward while gravity tries to pull it back in.
These are the beginnings of dust grains. This dust then continues outward still driven by radiative pressure cooling further and growing larger. At some point the particle density becomes low enough that the grains will not become significantly larger. Theoretical work on dust grain synthesis and populations abounds, but observations have thus far not allowed a good statistical understanding of dust creation. The ultimate aim of our study is to create just such a statistical base so that trends can be seen.