Identification of Silicon Line Emission in the Solar Extreme Ultraviolet Spectrum and Comparison with Theory and Astrophysical Observations

Details Identification of Silicon Line Emission in the Solar Extreme Ultraviolet Spectrum and Comparison with Theory and Astrophysical Observations Identification of Silicon Line Emission in the Solar Extreme Ultraviolet Spectrum and Comparison with Theory and Astrophysical Observations

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1308b&link_type=abstract

American Astronomical Society, SPD meeting #40, #13.08; Bulletin of the American Astronomical Society, Vol. 41, p.833

Astronomy and Astrophysics

Astronomy

Scientific paper

We have been re-evaluating the solar EUV spectra in the 20 - 300 Å region in order to identify lines that previously have been classified as unknown (Hinteregger et al. 1981). Based on new laboratory measurements, theoretical calculations (Liang et al., 2008), and observations of these lines in the Chandra spectra of the solar analogue, Procyon, we have tentatively identified new silicon lines. Measurements of silicon (Si V- Si XII) were taken on the Lawrence Livermore electron beam ion trap EBIT-II in the wavelength range 30-120 Å. Calculations were performed using the Flexible Atomic Code. Making assignments of previously unassigned lines will provide valuable feedback to both solar and stellar physics.
Hinteregger, H. E., Fukui, K., & Gibson, B. R., 1981, Geophys. Res. Letters 8, 1147.
Liang, G. Y., & Zhao, G., 2008, MNRAS 384, 489.
This project was supported by NASA's Solar and Heliospheric Physics program under grant No. NNX07AH98G. Work at LLNL was performed under the auspices of DOE under contract DE-AC53-07NA27344 and supported by NASA's Astronomy and Physics Research and Analysis program under contract NNH07AF81I.

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