Iterative Tomography: A Key to Providing Time-Dependent 3-D Reconstructions of the Inner Heliosphere and the Unification of Space Weather Forecasting Techniques

Bernard V Jackson,Dusan Odstrcil,Lucas Cota,Richard Fallows,Mario M Bisi,Munetoshi Tokumaru,Andrew Buffington

doi:10.3389/fspas.2020.568429

Abstract

Over several decades, UCSD has developed and continually updated a time-dependent iterative three-dimensional (3-D) reconstruction technique to provide global heliospheric parameters—density, velocity, and component magnetic fields. For expediency, this has used a kinematic model as a kernel to provide a fit to either interplanetary scintillation (IPS) or Thomson-scattering observations. This technique has been used in near real time over this period, employing Institute for Space-Earth Environmental Research, Japan, IPS data to predict the propagation of these parameters throughout the inner heliosphere. We have extended the 3-D reconstruction analysis to include other IPS Stations around the Globe in a Worldwide Interplanetary Scintillation Stations Network. In addition, we also plan to resurrect the Solar Mass Ejection Imager Thomson-scattering analysis as a basis for 3-D analysis to be used by the latest NASA Small Explorer heliospheric imagers of the Polarimeter to Unify the Corona and Heliosphere mission, the All Sky Heliospheric Imager, and other modern wide-field imagers. Better data require improved heliospheric modeling that incorporates non-radial transport of heliospheric flows, and shock processes. Looking ahead to this, we have constructed an interface between the 3-D reconstruction tomography and 3-D MHD models and currently include the ENLIL model as a kernel in the reconstructions to provide this fit. In short, we are now poized to provide all of these innovations in a next step: to include them for planned ground-based and spacecraft instruments, all to be combined into a truly global 3-D heliospheric system which utilizes these aspects in their data and modeling.

Highlights

The bulk of the particles within the solar wind, a hot, strongly turbulent plasma produced by the Sun, are accelerated up to speeds of about 400 km s−1 or more
In the mid-2010s, we found that the 3-component fields derived through this technique could be interpreted at Earth on a daily basis to provide Geocentric Solar Magnetospheric (GSM) Bz fields to enable a several-day future prediction of minor to moderate Geomagnetic Storms (Jackson et al, 2019)
We show the preliminary analysis of this data set for density the May 30, 2003, Coronal Mass Ejections (CMEs) event sequence (Jackson et al, 2008a), shown in Figure 12, which required slightly over 33 h to provide this result on the AMD machine using 14.4% of the 512 Gigabyte memory, and this is clearly insufficient as a real-time system at the moment

Summary

Introduction

The bulk of the particles within the solar wind, a hot, strongly turbulent plasma produced by the Sun, are accelerated up to speeds of about 400 km s−1 or more. The UCSD tomographic analyses with a kinematic modeling kernel and ISEE IPS data quickly iterate to update the basic heliospheric plasma parameters, density, velocity, and magnetic field.

Results

Conclusion