Solar emission lines revisited - Extended study of magnesium

Details Solar emission lines revisited - Extended study of magnesium Solar emission lines revisited - Extended study of magnesium

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phys...35..792c&link_type=abstract

(Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysics and Fusion Research, 2nd, Toledo, OH, Aug. 1986) Physica

Astronomy and Astrophysics

Astrophysics

19

Chromosphere, Emission Spectra, Magnesium, Solar Spectra, Fine Structure, Infrared Radiation, Polarized Electromagnetic Radiation, Rydberg Series

Scientific paper

Edlen's polarization formula is found to fit the high-l solar infrared emission lines attributed to Mg I to the accuracy of the high-precision observations. For several previously unidentified weak lines, assignments are made, a few to Mg I. With some revision of laboratory energy levels, a more precise ionization limit for Mg I is determined to be 61,671.056 (10)/cm. The fine structure of the two strongest lines at 811 and 818/cm is found to consist of 4 components spaced about 0.001/cm apart with nearly equal intensities. Their behavior in the penumbra magnetic field is well described by the Paschen-Back effect. Their line profile, polarization, and directional properties are discussed.

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