Exploring large-scale coronal magnetic field over extended longitudes by STEREO/EUVI and its effect on solar wind prediction

Details Exploring large-scale coronal magnetic field over extended longitudes by STEREO/EUVI and its effect on solar wind prediction Exploring large-scale coronal magnetic field over extended longitudes by STEREO/EUVI and its effect on solar wind prediction

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh23a..06n&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH23A-06

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2169 Solar Wind Sources, 7509 Corona, 7524 Magnetic Fields

Scientific paper

The potential field source surface (PFSS) model forms the basis of a wide range of heliospheric science and applications, including prediction of the solar wind speed near Earth. Experience shows that the model sometimes works quite well, but not always. Possible reasons for failure include deviation of the interplanetary magnetic field from the nominal Parker spiral, violation of the assumptions used in the model such as the discontinuity at the source surface, and the lack of simultaneous full-surface magnetograms. Here we study the impact of the lack of simultaneous full-surface magnetograms, using observations of the corona over an extended longitude range made possible by the EUVI on board the STEREO mission. In spite of the lack of magnetographs on STEREO, EUVI data with a growing separation angle between spacecraft A and B at least allow us to locate major active regions and coronal holes in the area not seen from Earth. The PFSS extrapolations and their input synoptic maps are compared with EUVI data to measure how well the model fits the observations. These comparisons are discussed in terms of the solar wind speed predicted by the model and observed at L1 by ACE.

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