Physics
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21349201a&link_type=abstract
American Astronomical Society, AAS Meeting #213, #492.01; Bulletin of the American Astronomical Society, Vol. 41, p.471
Physics
Scientific paper
Solar coronal and solar wind models are becoming more sophisticated as they are developed with realistic physics that describe the heating and acceleration processes in the corona. In the past these models have been tested by comparing their outputs with solar wind data (densities, temperatures, and outflow velocities) measured at 1 AU. In this paper we use spectroscopic data from the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) to compare with the outputs of a specific solar coronal model. The model selected was the Solar Corona component from the Michigan SpaceWeather Modeling Framework (SWMF). Specifically we use the observed $1/e$ profile line widths of HI Ly-alpha to compare with the plasma temperatures predicted by the
model. The comparisons are made in the corona at heights between 1.5Ro and 3.5Ro during the solar minimum of Cycle 23. We find that there are areas where the model can be improved, especially in the coronal hole regions over the poles of the Sun. This work is supported in part by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568 and by the Smithsonian Institution.
Anderson India
Stacy John Gregory
Strachan Leonard
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