Effects of Far-side Evolution of Magnetic Structures on Coronal and Interplanetary Magnetic Features

Models for the structure and dynamics of the corona and the interplanetary medium are based on magnetic boundary conditions at the Sun's surface. The degree to which this magnetic boundary condition faithfully represents the actual conditions at the Sun's surface will obviously influence how well the models can accurately reproduce the conditions in the interplanetary medium. Here we show how incorporating the evolution of far-side magnetic structures (including far-side active regions) affects the structure of the corona and solar wind. We compare observations of coronal structures (coronal holes) with those produced from: 1) synoptic magnetic maps with no far-side evolution; 2) synchronic maps in which the near-side magnetic structures evolve on the far-side via our Advective Flux Transport (AFT) code; and 3) synchronic maps with far-side evolution via the AFT code incorporating far-side information from STEREO EUV images. We will likewise compare observations of solar wind magnetic structures with those produced with these three different boundary conditions.