A Temperature and Density Model of the Solar Corona

Details A Temperature and Density Model of the Solar Corona A Temperature and Density Model of the Solar Corona

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.0404l&link_type=abstract

American Astronomical Society, SPD meeting #34, #04.04; Bulletin of the American Astronomical Society, Vol. 35, p.811

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We have developed the foundations of a 3-d global temperature and density model of the solar corona based on first principles. The method involves a static energy balance along individual coronal loops, with the heating term taken from a given coronal heating theory. We use the model to create synthetic emission images of active regions for comparison with observed X-ray and UV satellite images. The technique will enable us to perform a statistical study of active region heating with Yohkoh data from the last decade, comparing observations with the predicted emission measures and X-ray morphologies for different heating theories. The model is also useful for a variety of other applications, such as calculations of wave propagation and shock phenomena, testing of coronal magnetic field extrapolation techniques such as the potential and FFF models, and testing assumptions about the spatial distribution of heating along loops.
We have applied the technique to two cases: a simulated emerged active region, and NOAA active region 8210. These cases employ a heating term derived from the empirical relationship of Pevtsov et al. (2003) relating soft X-ray luminosity to total unsigned magnetic flux for a wide range of solar and stellar magnetic features. We present results from these two cases, including a comparison of the synthetic emission images of AR 8210 with Yohkoh SXT data. This work was supported by a DoD/AFOSR MURI grant, "Understanding Magnetic Eruptions and their Interplanetary Consequences."

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