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Proceedings Paper

High-n recombination lines in the solar atmosphere
Author(s): Bruna I. Grimberg; Edward Chang; Mark Heyer
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Paper 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.

Paper Details

Date Published: 19 August 1994
PDF: 8 pages
Proc. SPIE 2211, Millimeter and Submillimeter Waves, (19 August 1994); doi: 10.1117/12.183075
Show Author Affiliations
Bruna I. Grimberg, Univ. of Massachusetts/Amherst (United States)
Edward Chang, Univ. of Massachusetts/Amherst (United States)
Mark Heyer, Univ. of Massachusetts/Amherst (United States)


Published in SPIE Proceedings Vol. 2211:
Millimeter and Submillimeter Waves
Mohammed N. Afsar, Editor(s)

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