a Real-Time Global Solar Wind Boundary from Remotely-Sensed IPS Data for Use in 3D-MHD Modeling

The University of California, San Diego interplanetary scintillation (IPS) remote-sensing analyses of the heliosphere have regularly measured and reconstructed 3D solar wind structure for nearly two decades. This enables a real-time forecast of solar wind density and velocity that is nearly complete over the whole heliosphere with a time cadence of about one day. When using the IPS velocity analyses, we can accurately convect solar surface background magnetic fields outward and thus provide values of the field (radial and tangential components) throughout the global volume. The resulting precise time-dependent results extracted at any solar distance in the inner heliosphere can be further extrapolated outward to the edge of the heliosphere using current 3D-MHD modeling techniques. Here we present real-time determinations of these global solar wind analyses that can be used as an inner boundary to drive MHD models. Preliminary 3D-MHD forward-modeling results from two different modeling efforts (e.g., ENLIL, and HAF-3DMHD) are shown using recent IPS data sets. We explore the physical differences between the IPS observations and these current 3D-MHD modeling techniques. Our motivation is to ultimately provide a boundary to iteratively update any 3D-MHD model as frequently as new information near the Sun and from IPS data become available.