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