Measurement And Modeling Of Fe VIII To Fe XVI M-shell Emission In The Extreme Ultraviolet

Details Measurement And Modeling Of Fe VIII To Fe XVI M-shell Emission In The Extreme Ultraviolet Measurement And Modeling Of Fe VIII To Fe XVI M-shell Emission In The Extreme Ultraviolet

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2513b&link_type=abstract

American Astronomical Society Meeting 210, #25.13; Bulletin of the American Astronomical Society, Vol. 39, p.133

Physics

Scientific paper

The solar EUV emission near 200 Å is presently being studied with high resolution with the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS), which focuses on the emission between 90 and 270 Å, and with the EUV Imaging Spectrometer on Hinode, which focuses on the region 180 to 204 Å and 250 to 290 Å. The Solar EUV Experiment on the TIMED spacecraft also observes this spectral band but with greatly reduced resolution. The spectrum in this region is dominated by emission from moderate charge states of iron. The interpretation of the data relies on accurate and complete plasma emission models, notably CHIANTI. We have performed a series of laboratory measurements of the 3-3 emission from M-shell iron ions. The measurements cover the range 170 - 250 Å and are made at an electron density of about 1011 cm-3. Emission from Fe VIII through Fe XVI has been identified. Excellent agreement with CHIANTI predictions is found. A few weak transitions are noted in the laboratory data that are predicted by CHIANTI to be vanishingly small and should not have been observed. These are tentatively attributed to transitions in Fe XV. A comparison with observations from CHIPS is also presented.
This work was supported in part by NASA's Solar and Heliospheric Physics Supporting Research and Technology Program. Work at UC-LLNL was performed under the auspices of the DOE by under Contract W-7405-Eng-48.

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