Hyperfine Structure in the Solar Spectrum

The hyperfine structure of certain lines can be detected in the solar spectrum as reproduced in the Utrecht atlas; it can contribute appreciably to the width of the lines. The agreement between the predicted and observed half-widths and profiles of lines with hyperfine structure broadening is good. Solar lines with wide hyperfine structure patterns show a wave-length shift toward the weak end of the pattern as compared to the laboratory wave length. Hyperfine broadened lines fall on a different curve of growth, characterized by a larger Doppler velocity and a smaller damping constant. A resum of the elements most affected by hyperfine broadening is given.