Detailed models of disks around young low-mass stars are essential to understand the formation and further evolution of earth-like planets and provide the necessary frame work for the generation and maintenance of habitable zones.
This subproject focuses on novel numerical computations of axisymmetric inner and outer disk models based on the interaction of gas, radiation fields and dust particles. An implicit adaptive grid approach allows numerical computations over spatial regions where the sound velocity as well as the orbital speed of the gas can vary over many orders of magnitude. Stellar radiation and stellar winds are important factors in shaping the stellar environment when they interact with the circumstellar disk. Rapid changes of the radiation field (e.g. FU Orionis outbursts, stellar flares, etc.) as well as variations in the stellar wind properties generate e.g. shock waves or ionization fronts propagating through the disk thereby heating, evaporating and ionizing the gas-dust mixture, changing the structure and shape of dust particles and chemically processing the gas.