Quick interpretation of unresolved hyperfine and/or Zeeman structures in stellar spectra

Details Quick interpretation of unresolved hyperfine and/or Zeeman structures in stellar spectra Quick interpretation of unresolved hyperfine and/or Zeeman structures in stellar spectra

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jphys..49..263b&link_type=abstract

(IAU, ESA, CNRS, et al., Colloquium on UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, 102nd, Beaulieu-sur-Me

Astronomy and Astrophysics

Astrophysics

2

Hyperfine Structure, Stellar Atmospheres, Stellar Spectra, Zeeman Effect, Angular Momentum, Emission Spectra, Forbidden Bands, Nuclear Spin, Spectral Line Width, Stellar Magnetic Fields

Scientific paper

Some atomic or ionic lines emitted by stellar atmospheres are very useful clues for estimating the local magnetic fields. However, their use is often complicated by insufficient experimental resolution and by the occurrence of hyperfine structure. Here, the average wavelength and the width of the component set corresponding to each type of polarization are given by compact formulas, in terms of the magnetic field, and of the Lande factors and hyperfine magnetic and electric constants of both involved levels.

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