On the extreme ultraviolet solar emission of B-like ions - O IV

Details On the extreme ultraviolet solar emission of B-like ions - O IV On the extreme ultraviolet solar emission of B-like ions - O IV

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....45..145f&link_type=abstract

Astronomy and Astrophysics, vol. 45, no. 1, Dec. 1975, p. 145-150.

Astronomy and Astrophysics

Astrophysics

104

Electron Scattering, Far Ultraviolet Radiation, Oxygen Ions, Solar Radiation, Transition Probabilities, Electron Energy, Electron Orbitals, Electron Transitions, Emission Spectra, Ionic Collisions, Oxygen Spectra, Radiant Flux Density

Scientific paper

Radiative transition probabilities and collision strengths are calculated in intermediate coupling for relevant transitions between the 2s(2)2p, 2s2p(2), and 2p(3) configurations of O(3+) as an aid in interpreting the observed relative intensities of the O IV lines in the solar EUV spectrum. The emissivities of the O IV lines at 790, 788, 625, and 609 A are computed relative to the 554-A line on the basis of the results. The emissivity ratios are compared with observed intensity ratios, and the line intensities are compared with observed absolute line intensities. The calculations are found to be consistent with the observations and with previous calculations of the O(3+) ionization equilibrium. When extended to include the O V and O VI resonance lines, the analysis shows that the function chi is constant over the electron-temperature range from 100,000 to 600,000 K, implying that the electron temperature and conductive flux vary in the same way throughout the chromosphere-corona transition region.

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