Poster abstract details

In the past few years, the origin of the myriad of morphologies presented by planetary nebulae has been extensively studied, based on observations and both analytical and numerical models. In the theoretical domain magnetic fields, jets and interacting winds have been proposed. However, these models have not been confronted with the observations except for density or column density maps. In order to perform a full analysis, comparing the models to the observations, the inclusion of ionization from a central source is mandatory. In this work we study the formation of asymmetric nebulae based on wind interaction + light jets, and perform a full 3D radiative transfer calculation to obtain a self-consistent distribution of ions. The emission maps for the main emission lines is obtained. Combining the emissivities with the simulated velocity distributions, we obtain position-velocity maps that may be directly compared to the observations.