New and Revised Line Assignments Among the Solar Iron Emission Lines

Details New and Revised Line Assignments Among the Solar Iron Emission Lines New and Revised Line Assignments Among the Solar Iron Emission Lines

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp51b..16b&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP51B-16

Physics

7509 Corona, 7549 Ultraviolet Emissions

Scientific paper

An investigation of the iron emission lines in the 170-210 Å region covered by the low-wavelength channel of the Extreme Ultraviolet Imager (EIS) on board the Hinode satellite revealed a discrepancy between the line list implemented in the CHIANTI code and that available from NIST. The lines at issue were from Fe XI, XII, and XIII. We resolved this discrepancy by conducting laboratory studies in which differing amounts of the relevant ions were produced and the line emission from each ionization state was recorded. These measurements have also found fifteen new, albeit weak, iron lines in the 170-240 Å region, which are absent from CHIANTI. The lines are attributed mostly to Fe XIII. This work was supported by NASA's Solar and Heliospheric Physics Program award NNX07AH98G. Work at LLNL was performed under the auspices of the U.S. DOE under Contract DE-AC52-07NA27344.

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