During the solar minimum STEREO observations show that the three-dimensional structure of the solar corona can be described well by a tilted bi-polar magnetic configuration. The slow solar wind is modeled using three-fluid model that includes heavy ions, such as He II and O VI. The model is initialized with dipole magnetic field and spherically symmetric density. The resulting steady state non-potential and non-uniform streamer configuration calculated with this model is compared to STEREO observations of the streamer density structure. SOHO/UVCS observations are used to compare the O VI emission to model results. We discuss the unique properties of the solar wind produced in this configuration.
@article{arxiv.1004.4847,
title = {Modeling the slow solar wind during the solar minimum},
author = {Leon Ofman and Maxim Kramar},
journal= {arXiv preprint arXiv:1004.4847},
year = {2010}
}