Prediction of Solar Wind Conditions in the Inner Heliosphere Using IPS Tomography

Details Prediction of Solar Wind Conditions in the Inner Heliosphere Using IPS Tomography Prediction of Solar Wind Conditions in the Inner Heliosphere Using IPS Tomography

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0241h&link_type=abstract

American Astronomical Society, SPD Meeting #31, #02.41; Bulletin of the American Astronomical Society, Vol. 32, p.818

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The ability to determine the 3D structure of the co-rotating component of the inner heliosphere, and of the 3D extent and evolution of solar disturbances superposed on this co-rotating background, are of primary importance for effective 'space weather' forecasting. We developed a tomographic technique that uses remote sensing data to reconstruct a heliospheric solar wind density and velocity model. This enables us to reconstruct the background solar wind as well as solar disturbances as they move away from the Sun, and forecast their subsequent arrival at Earth. Currently we are testing a real-time forecasting system based on tomographic reconstructions of the solar wind from interplanetary scintillation (IPS) data, available on a daily basis from the Solar Terrestrial Environment Laboratory (STE-Lab) near Nagoya, Japan. The IPS tomography is used to determine velocities at 1 AU where they are compared with in situ observations from Earth-orbiting spacecraft. The tomographic solar wind model is also used to passively 'convect' Stanford magnetic field data from the source outward to 1 AU for comparison with in situ magnetic field data. We show current results from this IPS forecasting system. The real-time forecasting data are available on a dedicated Web site at http://casswww.ucsd.edu/personal/bjackson/weather.htm. This work was supported by NSF grant INT-9815377 and AFOSR grant AF49620-97-1-0070.

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