Using IPS Magnetic Modeling to Determine Bz

Tuesday, 16 December 2014
Bernard V Jackson1, Hsiu-Shan Yu2, P. Paul Hick2, Andrew Buffington2, Julio Cesar Mejia-Ambriz2, Mario Mark Bisi3 and Munetoshi Tokumaru4, (1)University of California San Diego, Center for Astrophysics and Space Science, La Jolla, CA, United States, (2)University of California San Diego, La Jolla, CA, United States, (3)Rutherford Appleton Laboratory, Didcot, OX11, United Kingdom, (4)Nagoya University, Nagoya, Japan
Interplanetary scintillation (IPS) observations enable remote determinations of velocity and density in the inner heliosphere while also providing forecasts of these quantities. Using the global velocities inferred from IPS, and through convection upward of magnetic fields perpendicular to a source surface produced by the Current–Sheet Source Surface (CSSS) modified potential model (Zhao and Hoeksema, J. Geophys. Res., 100, 19, 1995), global long-duration radial and tangential heliospheric field components can also be determined. In order to better include short-term transient effects and derive a value for the field normal to these components (Bn) during periods where CMEs, are present, we have tested an extension to our current 3D vector-field analysis. This extension adds closed fields from below the source surface to the CSSS model values, and when traced outward from the sub-Earth point, three magnetic field components are present. These are compared to in-situ magnetic fields measured near Earth for several periods throughout the current solar cycle from the minimum between Solar Cycle 23 and 24 up until the present. We find a significant positive correlation when using this extension to current analyses including that of the Bn field for the test cases analyzed thus far.