Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...521..839d&link_type=abstract
The Astrophysical Journal, Volume 521, Issue 2, pp. 839-843.
Astronomy and Astrophysics
Astronomy
13
Atomic Processes, Line: Formation, Line: Identification, Sun: Corona, Sun: X-Rays, Gamma Rays
Scientific paper
The identification of the emission-line feature at 17.62 Å in solar X-ray spectra is reexamined. Using a Monte Carlo technique, we compute a realistic theoretical upper limit to the observed Fe Lalpha photospheric fluorescent line strength caused by irradiation from an overlying corona. These calculations demonstrate that the photospheric Fe Lalpha characteristic line is much too weak to account for the observed 17.62 Å line flux. Instead, we identify this line with the configuration interaction 2s^22p^43p^2P_3/2-2s2p^6^2S_1/2 transition in Fe XVIII seen in Electron Beam Ion Trap spectra and predicted in earlier theoretical work on the Fe XVIII X-ray spectrum. This line should be easily resolved and detected in stellar coronae by the spectrographs on the upcoming Chandra X-ray Observatory and X-ray Multimirror Mission.
Beiersdorfer Peter
Brown Gregory V.
Drake Jeremy J.
Kahn Steven M.
Swartz Douglas A.
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