High-n recombination lines in the solar atmosphere

Bruna I. Grimberg; Edward Chang; Mark Heyer

doi:10.1117/12.183075

19 August 1994 High-n recombination lines in the solar atmosphere

Bruna I. Grimberg; Edward Chang; Mark Heyer

Author Affiliations +

Proceedings Volume 2211, Millimeter and Submillimeter Waves; (1994) https://doi.org/10.1117/12.183075
Event: Millimeter and Submillimeter Waves and Applications: International Conference, 1994, San Diego, CA, United States

Abstract

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, Bruna I. Grimberg, Edward Chang, Edward Chang, Mark Heyer, Mark Heyer, } "High-n recombination lines in the solar atmosphere", Proc. SPIE 2211, Millimeter and Submillimeter Waves, (19 August 1994); doi: 10.1117/12.183075; https://doi.org/10.1117/12.183075

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