Comparison between All-Sky Images Observed by Satellite SMEI and Simulations by using the HAF Solar Wind Model

Details Comparison between All-Sky Images Observed by Satellite SMEI and Simulations by using the HAF Solar Wind Model Comparison between All-Sky Images Observed by Satellite SMEI and Simulations by using the HAF Solar Wind Model

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh41b0465s&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH41B-0465

Other

2102 Corotating Streams, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2139 Interplanetary Shocks, 7513 Coronal Mass Ejections, 7519 Flares

Scientific paper

The Solar Mass Ejection Imager (SMEI) is a new satellite in sun-synchronous, low earth orbit with three wide-angle, white light photometers that provides a scan of the celestial sphere every orbit. By occulting the sun and correcting for other sources, the 0.1% of total light scattered from the increased plasma density associated with the flare-induced shock may be revealed. The first observations from SMEI were a series of eighteen frames acquired after two solar flares on May 27th and 29th, 2003. The interplanetary consequences of these flares were numerically modeled using the Hakamada-Akasofu-Fry (HAFv.2) kinematic solar wind model. Line-of-sight plasma densities due to the background solar wind and to the two shock fronts were calculated and displayed in the Hammer-Aitoff reference frame to enable direct comparison with the SMEI observations. Comparison of the HAFv.2 simulation with the SMEI observations clearly demonstrates that the model is necessary to aid in the identification of multiple shock-induced variations and to remove the contribution of the background solar wind from the SMEI observations.

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