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Atmospheric Imaging Assembly Response Functions: Solving the Fe VIII Problems with Hinode EIS Bright Point Data View all abstracts by submitter

Joan Schmelz   Submitted: 2013-01-09 10:23

The Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory is a state-of-the-art imager with the potential to do unprecedented time-dependent multi-thermal analysis at every pixel on scales short compared to the radiative and conductive cooling times. Recent results, however, have identified missing spectral lines in the CHIANTI atomic physics data base, which is used to construct the instrument response functions. This is not surprising since the wavelength range from 90 ? to 140 ? has rarely been observed with solar spectrometers, and atomic data for many of these ions are simply not available in the literature. We have done differential emission measure analysis using simultaneous AIA and Hinode/EIS observations of six X-ray bright points. Our results not only support the conclusion that CHIANTI is incomplete near 131 Å, but more importantly, suggest that the peak temperature of the Fe VIII emissivity/response is likely to be closer to log T = 5.8 than to the current value of log T = 5.7. Using a revised emissivity/response calculation for Fe VIII, we find that the observed AIA 131-? flux can be underestimated by ~1.25, which is smaller than previous comparisons. Making these adjustments brings not only the AIA 131-? data but also the EIS Fe VIII lines into better agreement with the remainder of the bright point data. In addition, we find that CHIANTI is reasonably complete in the AIA 171- and 193-? bands. For the AIA 211-, 335-, and 94-? channels, we recommend that more work be done with AIA?EIS DEM comparisons using observations of active region cores, coronal structures with more warm emission measure than our bright points. Then direct comparisons can be made with a variety of EIS iron lines.

Authors: J.T. Schmelz, B.S. Jenkins, J.A. Kimble
Projects: SDO-AIA

Publication Status: Solar Physics, 2013, DOI 10.1007/s11207-012-0208-1
Last Modified: 2013-01-09 10:40
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