Relative intensities of singlet and triplet lines of Hei in the solar chromosphere allow a determination of bn exp E~n/Te~, where ~,` is the ionization energy of the level n and bn is a non- thermodynamic equilibrium factor. We have computed bn'5 for values of Te ranging from 10,0000 to 50,0000 for an idealized helium atom consisting of a continuum and IS level and the levels 25, 2P, and n = 3, 4 and 5 in the excited singlets and triplets. Computed and observed values of b exp E~n/Te~ for the triplets agree for all Te even though b varies with Te. The relative populations of the triplets are determined almost entirely by the radiative transitions, which, because of the low chromospheric opacity in the triplets, are independ~nt of the ambient Te. For the singlets, however, the occupation numbers of the excited levels depend critically upon R~, the net radiative transition rates to the ground state, which are functions of TO, the chromospheric opacity in the first resonance line. Thus, both Te and TO are parameters of the calculations, with TO, in turn, being a function of Te and ne. The electron density, ne, may be estimated from the absolute line intensities. In order to relate Re to TO, we use the source- function computations of Jefferies and Thomas (1959). Computed values of be exp E~n/Te~ and TO for the singlets agree satisfactorily with the empirical be exp E~.~/Te~ for Te 4o,ooo0~5o 0000 Uncertainties in atomic constants and Rn may permit a Te as low as 30,0000, but certainly not as low as 25,0000. At chromospheric densities, helium becomes predominantly Heii at Te 20,000, and predominantly Heiii at Te 55,ooo0. Chromospheric helium is, there- fore, predominantly Heii as suggested earlier by Athay and Menzel (1956). REFERENCES Athay, R. G. and Meuzel, D. H. 1956, Ap. J. 123, 285. Jefferies, J. T. and Thomas, R. N. 1959, Ap. J. 129, 401. National Bureau of Standards and High A ltitude Observatory Boulder, Colorado
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