Modeling of the EUV/Soft X-ray Emission in a Large Coronal Bright Point

Details Modeling of the EUV/Soft X-ray Emission in a Large Coronal Bright Point Modeling of the EUV/Soft X-ray Emission in a Large Coronal Bright Point

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0126b&link_type=abstract

American Astronomical Society, SPD meeting #37, #1.26; Bulletin of the American Astronomical Society, Vol. 38, p.219

Astronomy and Astrophysics

Astronomy

Scientific paper

We use potential field extrapolations of SOHO/MDI and Kitt Peak Vacuum Telescope high resolution magnetograms to model the magnetic field line distribution in a large coronal bright point. We populate the field lines with solutions to the hydrostatic loop equations and simulate the emission observed at EUV and soft X-ray wavelengths. The results are compared in detail to observations obtained by Yohkoh/SXT, SOHO/EIT, and SOHO/CDS. Previous similar studies of larger active regions have shown that relatively good agreement is obtained between the simulated and observed soft X-ray images. The simulations, however, fail to correctly model the loop emission and integrated intensities at EUV wavelengths simultaneously. Our results support these conclusions; the SXT images and integrated intensities agree well with the observations, but the spatial distributions of the EUV line intensities are incorrect even when the integrated intensities are correct. We further extend the analysis to lines formed in the transition region. Here the simulated intensities are too large by factors of 2--4 and there are differences in the morphology of the network emission. We explore the consequences for these comparisons of using loop expansion and different forms of the heating function in the models. The techniques are also applied to model the on-disk and off-limb intensities in the quiet corona.This research was supported by the NASA Guest Investigator Program and the Office of Naval Research.

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