Stream Structure and Coronal Sources of the Solar Wind During the May 12th, 1997 CME

Details Stream Structure and Coronal Sources of the Solar Wind During the May 12th, 1997 CME Stream Structure and Coronal Sources of the Solar Wind During the May 12th, 1997 CME

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42b0523a&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH42B-0523

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2134 Interplanetary Magnetic Fields, 2169 Sources Of The Solar Wind, 7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields

Scientific paper

We report on our efforts to model the ambient solar wind out to 1AU around the time of the May 12th 1997 Halo CME and to identify its coronal source regions. We use three different coupled coronal/solar wind models to accomplish this: the simple physics and empirical based Wang-Sheeley-Arge (WSA) model, the advanced 3-D Magnetohydrodynamic (MHD) ENLIL solar wind model coupled to results generated by the SAIC 3-D steady state MHD coronal model, and the magnetostatic coronal component of the WSA model coupled to the ENLIL model. In addition, the sheath region of the ICME event is simulated using the ENLIL 3D MHD code by launching an over pressured hydrodynamic cloud with speed, extent, duration, and position determined by the Zhao Cone model [Zhao et al., JGR, 2001]. The simulation results generated by the different model combinations are then compared with the WIND satellite observations near Earth as well as with each other. We find that all three coupled models describe the ambient solar wind stream structure around the time of the May 12th, 1997 CME generally well, except for the ejecta itself, as evidenced by the overall good agreement between the solar wind observations at L1 and model simulation results, which are themselves in surprisingly good agreement with each other. The ENLIL model successfully replicates the ambient solar wind plus the shock and sheath region of the ICME when a simple over pressured hydrodynamic cloud is applied. Our results suggest that the source of the high-stream that followed the CME originated from a coronal hole extension located south of the Sun's equator.

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