Proton excitation rates for fine structure transitions in C III, O V, and NE VII in the sun

Details Proton excitation rates for fine structure transitions in C III, O V, and NE VII in the sun Proton excitation rates for fine structure transitions in C III, O V, and NE VII in the sun

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....90...97d&link_type=abstract

Astronomy and Astrophysics, vol. 90, no. 1-2, Oct. 1980, p. 97-101. Research supported by the Department of Education of Northe

Astronomy and Astrophysics

Astrophysics

39

Carbon, Collision Rates, Electron Transitions, Fine Structure, Oxygen, Solar Protons, Abundance, Atomic Energy Levels, Neon, Plasma Diagnostics, Proton Impact

Scientific paper

The close-coupled impact parameter method is used to calculate the proton excitation rates for fine structure transitions in the levels (2s, 2p) 3P and (2p)2 3P of the ions C III, O V, and Ne VII. By the use of these proton rates and recently calculated electron collision rates, the effect of these proton rates on line ratios involving these fine structure levels has been studied at electron temperatures and densities appropriate to the solar transition region. Theoretical estimates of the strength of the (2s, 2p) 3P (2s)2 1S line are only slightly affected by the inclusion of proton rates. The estimate of the strength of the multiplet is decreased by 10% in the case of O V and Ne VII at the temperature of maximum abundance and 25% for higher temperatures.

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