CISM

SOHO image animation (57k)
images from SOHO-EIT

Reconstruction of the Solar/Interplanetary Disturbances for the Space Weather Event on 6-10 Jan 1997

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The MHD solar wind model will describe all of the key solar wind parameters around the time of arrival of the modeled coronal transient-induced disturbance on 10 Jan 1997. This description will include the overall magnetic geometry, the preceding interplanetary shock and piled-up solar wind, and the distortion of the ejecta by the surrounding solar wind streams. The simulation of any high density features related to the filament disruption will require a more advanced model that merges the coronal mesoscale structure with the global coronal and solar wind models. (This image shows evolution of an ejected high density pulse from the HD model at SEC. It illustrates the basic scenario that must be treated in the MHD model.) Click on the image to the right to see the corresponding animation.
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Successful replication of the WIND data validates the model(s). (The figure shows the solar wind measurements from the WIND Berkeley 3-D plasma experiment, and the Goddard Space Flight Center magnetometer for the 10 Jan 97 magnetic cloud.) Click on the image on the right to enlarge.

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