- Conference date: 19–23 March 2012
- Location: Palm Springs, CA, USA
At UCSD, remote-sensing analyses of the inner heliosphere have been regularly carried out using interplanetary scintillation (IPS) data for almost two decades. These analyses have measured and reconstructed 3D solar wind structure throughout this time period. These global results, especially using Solar-Terrestrial Environment Laboratory (STELab) IPS observations, provide time-dependent density and velocity that is nearly complete over the whole heliosphere for the major part of each year and with a time cadence of about one day. When using the volumetric velocity from this time-dependent tomography, we can accurately convect solar surface magnetic fields outward and thus provide values of the magnetic field throughout the global volume. We can extract a "boundary" at any height in the inner heliosphere from this analysis. These extrapolations also allow us to trace the magnetic connection of any heliospheric location back to the inner boundary surface as an approximation to the propagation path of the solar energetic particles. Here we present sample determinations of these global solar wind boundaries from recent IPS data, and provide some of the details that allow the interpolation of these boundary values across the STELab data "outage" periods.
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