Models of mass flows from cool, luminous stars

We have modeled the flow of gas and pargicles from cool, luminous stars, taking account of the radiative properties of the gas as well as the particles. We find that mass flows in which the particles have the optical characteristics of clean silicate material do not, in general, have energy distributions with conspicuous 10 μm excesses. However, clean silicate models having relatively warm particle shells do have distinct 10μm excesses. Flows with diry silicate particles are warm and generally display conspicuous 10 μm excesses. We also find that strong 2.7 μm water vapor absorption may be diagnostic of stars with relatively large luminosities and mass loss rates