Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.278..773k&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 278, Issue 3, pp. 773-780.
Astronomy and Astrophysics
Astronomy
17
Atomic Data, Sun: Activity, Sun: Flares, Ultraviolet: General
Scientific paper
Many intensity ratios involving FeXII 3s^23p^3-3s3p^4 and 3s^23p^3-3s^23p^23d transitions in the 186-383A wavelength range are known to be sensitive to electron density. We compare calculations for these lines with observations of a solar active region and of a subflare obtained during the 1989 flight of the Solar EUV Rocket Telescope and Spectrograph (SERTS). Electron densities derived from the majority of such ratios are consistent with one another for both solar features, and are also in good agreement with the values of N_e estimated from diagnostic lines in other species formed at similar electron temperatures to FeXII, such as FeXIII and FeXIV. These results provide observational support for the general accuracy of the diagnostic calculations, and imply that they may be applied to future observations planned with the Coronal Diagnostic Spectrometer on the SOHO mission. In addition, our analysis indicates that the line at 283.70A in the active region data is the 3s^23p^3 ^2D_3/2-3s3p^4 2P_1/2 transition in FeXII, the first time (to the best of our knowledge) that this line has been identified in the solar spectrum. Five of the line ratios considered are predicted to be relatively insensitive to the adopted electron temperature and density, and the good agreement found between theory and observation for three of these provides evidence for the reliability of the SERTS instrument calibration. However, for one of the remaining ratios the large discrepancies between theory and observation cannot be attributed to blending, and may be due to errors in the adopted atomic data.
Brown Paul J. F.
Foster John V.
Keenan Francis P.
Neupert Werner M.
Tayal Swaraj S.
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