High N solar radio recombination lines

Details High N solar radio recombination lines High N solar radio recombination lines

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...52..423g&link_type=abstract

Solar Physics, vol. 52, May 1977, p. 423-427.

Physics

2

Line Spectra, Pressure Broadening, Radiative Recombination, Solar Atmosphere, Solar Radio Emission, Spectral Line Width, Absorption Spectra, Chromosphere, Doppler Effect, Microwave Emission, Solar Spectra

Scientific paper

For a representative set of atmospheric and atomic parameters, the strengths of solar dielectronic recombination lines originating in ions with Z not exceeding 6 at frequencies of at least 70 GHz are determined. The derived line strengths are compared with those calculated by Berger and Simon (1972), and it is found that the present values for representative ions with Z not exceeding 3 are lower by a factor of 100 to 1000, being mainly the result of the inclusion of electronic pressure broadening. Requirements are outlined for the detection of lines, which must establish an upper limit of at least about 0.00001 for the line-to-continuum ratio.

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