EUV emission lines of O IV observed in solar spectra by the S-055 instrument on Skylab.

Details EUV emission lines of O IV observed in solar spectra by the S-055 instrument on Skylab. EUV emission lines of O IV observed in solar spectra by the S-055 instrument on Skylab.

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...306..621o&link_type=abstract

Astronomy and Astrophysics, v.306, p.621

Astronomy and Astrophysics

Astrophysics

5

Atomic Data, Sun: Uv Radiation

Scientific paper

Recent calculations of electron and proton impact excitation rates in O IV are used to derive the intensity ratios of lines in the ~340-1350A wavelength range as a function of electron temperature (T_e_) and density (N_e_). These results are presented in the form of ratio-ratio diagrams, which should in principle allow both N_e_ and T_e_ to be deduced for the O IV line emitting region of a plasma. Electron temperatures derived from ratio-ratio diagrams involving the 790A/554A ratio, in conjunction with observational data for several solar features obtained with the Harvard S-055 spectrometer on board Skylab, are found to be in reasonable agreement with the value of T_e_ expected from ionization equilibrium calculations. This provides some support for the theoretical diagnostics presented in this paper, and hence the atomic data used in their derivation. However other temperature and density sensitive ratios involving the O IV multiplets at 609A, 625A and 787A could not be used to derive plasma parameters from the ratio-ratio diagrams, due to blending with lines of Mg X and S V.

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