Statistics – Applications
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..150...61k&link_type=abstract
Solar Physics, vol. 150, no. 1-2, p. 61-70
Statistics
Applications
2
Applications Of Mathematics, Atomic Excitations, Electron Density (Concentration), Electron Energy, Emission Spectra, Line Spectra, Mathematical Models, Ratios, Solar Activity, Solar Spectra, Ultraviolet Astronomy, Ultraviolet Spectra, Logarithms, Matrices (Mathematics), Plasmas (Physics), Skylab Program, Solar Corona, Solar Transition Region, Spectroscopy
Scientific paper
Recent R-matrix calculations of electron impact excitation rates in O V are used to derive the emission line intensity ratios (in energy units) R1 = I(2s2p(sup3)P - 2p23P)/I(2s21S0 - 2s2p1P1 = I(761.1 A)/I(629.7 A), R2 = I(2s21S0 - 2s2p3P1/I(2s21S0 - 2s2p1P1 = I(1218.4 A)/I(629.7 A), and R3 = I(2s2p(sup1)P1 - 2p21S0/I(2s21S0 - 2s2p1P1) = I(774.5 A)/I(629.7 A) as a function of electron temperature (Te) and density (Ne). These results are presented as plots of R1 vs R2, and R1 vs R3, which should allow both Ne and Te to be deduced for the O V line emitting region of a plasma. Electron densities derived from the (R1, R2) and (R1, R3) diagrams in conjunction with observational data for several solar features obtained with the Harvard S-055 spectrometer on board Skylab are found to be compatible, and in good agreement with values of Ne estimated from line ratios in species formed at similar electron temperatures to O V. In addition, values of Te determined from (R1, R2) and (R1, R3) are generally close to that expected theoretically. These results provide experimental support for the accuracy of the diagnostic calculations presented in this paper, and hence the atomic data used in their derivation.
Berrington Keith A.
Doyle Gerry J.
Keenan Francis P.
Kingston A. E.
Warren G. A.
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