Synthetic photometry for carbon-rich giants. V.

This, in turn, is believed to be caused by radiation pressure due to the absorption and scattering of the stellar radiation by the dust grains formed in the atmosphere. The optical properties of dust are often estimated using the Small Particle Limit (SPL) approximation, and it has been used frequently in modelling AGB stellar winds when performing RHD (Radiation-HydroDynamics) simulations.

Here we investigate the effects of replacing the SPL approximation by detailed Mie calculations of the size-dependent opacities for grains of amorphous carbon forming in C-rich AGB star atmospheres. We have performed RHD simulations for a large grid of carbon star atmosphere+wind models with different effective temperatures, luminosities, stellar masses, carbon excesses and pulsation properties. Also, a posteriori radiative transfer calculations for many radial structures (snapshots) of these models were done resulting in spectra and filter magnitudes.