Other
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsa51b0236s&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SA51B-0236
Other
7519 Flares, 7524 Magnetic Fields, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks
Scientific paper
An interplanetary shock is often followed by a magnetic cloud. It is believed that magnetic clouds are related to halo-CMEs observed by SOHO/LASCO. Flare and erupting filament observations are used to locate the source on the solar surface. The Hakamada-Akasofu-Fry (HAFv2) solar wind model is used to calculate the shock arrival time, which can then be compared to shocks observed near Earth for the event on May 12, 1997. In order to fit the observed IMF configuration in the magnetic cloud that follows a shock, a magnetic cloud model is made and the force-free magnetic field model is applied inside the cloud. The velocity of the cloud is obtained on the basis of the average velocity of the shock from the HAF model. A three-dimensional configuration of interplanetary magnetic field lines, including the magnetic cloud, is obtained as a function of time. The simulated IMF using the combined models is in good agreement with solar wind observations near Earth. Several other examples are examined in the same way.
Akasofu Syun
Deehr Charles
Dryer Murray
Fry Craig D.
Smith Zdenka
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