Modeling the Corona and Solar Wind Using Polar Field Corrected Synoptic Maps

Details Modeling the Corona and Solar Wind Using Polar Field Corrected Synoptic Maps Modeling the Corona and Solar Wind Using Polar Field Corrected Synoptic Maps

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1107a&link_type=abstract

American Astronomical Society, SPD meeting #37, #11.07; Bulletin of the American Astronomical Society, Vol. 38, p.240

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Measurements of the line-of-sight (LOS) photospheric field near the Sun's poles are often highly unreliable because of their close proximity to the limb (i.e., only a small component of the field vector is directed toward the observer) and because the Sun's rotation axis is inclined 7.25° to the ecliptic plane. Regions located within 7.25° of the poles are in fact not even observable from Earth for up to six months at a time. The least reliable LOS photospheric field measurements thus tend to be those located near the poles. Photospheric field observations serve as a key driver to all coronal and solar wind models. These models (both simple and advanced) are especially sensitive to the field values at the Sun's poles, and therefore, it is crucial that they are determined as reliably as possible. In this study, we apply a polar field correction technique that we have developed [Arge and Pizzo, 2000] to a solar cycles worth of LOS photospheric magnetic field Carrington maps from Mount Wilson Solar observatory. We then use both the polar corrected as well as the uncorrected maps in the Wang-Sheeley-Arge (WSA) model, which is a simple physics and empirical based coronal and solar wind model. The WSA solar wind predictions at L1 are then compared with each other as well as with the observations from the WIND and ACE spacecraft.

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