Physics
Scientific paper
Oct 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...44..371g&link_type=abstract
Solar Physics, vol. 44, Oct. 1975, p. 371-382.
Physics
4
Hydrogen Recombinations, Solar Spectra, Spectral Line Width, Zeeman Effect, Electron Impact, Fine Structure, Frequency Response, H Alpha Line, Solar Magnetic Field
Scientific paper
The Zeeman broadening of high-n lines is derived. While the upper boundary of the observable frequency region of recombination lines is defined by electron-impact broadening, in areas of the quiet sun with field strengths of about 1 G, the Zeeman broadening will shift this boundary to higher frequencies in active regions with field strengths of at least about 25 G. The frequency region most favorable for observations is derived, and the corresponding Doppler, electron impact, and Zeeman broadening are discussed. The strengths of the recombination lines obtained in earlier calculations is reduced when one considers the electron-impact and Zeeman broadening in addition to the Doppler broadening. The frequency region favorable for observations is compared with the atmospheric transparency of the microwave region; it is found that observations require at least high-altitude stations or space-based platforms. Details are given for using the Zeeman broadening of high-n recombination lines for mapping (coronal) magnetic fields.
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