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19 August 1994High-n recombination lines in the solar atmosphere
The investigation of radio recombination lines if HI and heavier elements is one of the principal methods of studying the structure within the lower solar atmosphere. Spectral lines at millimeter wavelength may be formed in the solar chromosphere when Rydberg transitions between highly excited levels occur. Theoretical and observational antecedents to radio-frequency lines in the solar spectrum are summarized. Physical mechanisms that affect excited atoms immersed in a plasma are discussed and preliminary calculations of the relative line intensity for hydrogen recombination lines from H5(alpha) (7.46 micrometers ) to H42(alpha) (3.38 mm) are presented.
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Bruna I. Grimberg, Edward Chang, Mark Heyer, "High-n recombination lines in the solar atmosphere," Proc. SPIE 2211, Millimeter and Submillimeter Waves, (19 August 1994); https://doi.org/10.1117/12.183075