The MGI 8806A Line in the Spectra of Late Type Giant Stars

Details The MGI 8806A Line in the Spectra of Late Type Giant Stars The MGI 8806A Line in the Spectra of Late Type Giant Stars

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...277..165r&link_type=abstract

Astronomy and Astrophysics, Vol. 277, NO. 1/SEP(III), P. 165, 1993

Astronomy and Astrophysics

Astrophysics

6

Atomic Data - Stars: Abundances - Stars: Giant - Stars: Individual: Γ Tau, Μ Leo, Μ Peg

Scientific paper

Revised values for the oscillator strength and radiative width of the Mg I 8806 Å line are determined by reference to laboratory measurements and recent calculations. The unusually large radiative width is the dominant factor causing broadening of the line wings in the spectra of late-type giant stars. As a result, the line wings are insensitive to surface gravity but sensitive to metallicity. Profiles computed using the revised atomic data, appropriate stellar atmospheric parameters, and taking full account of CN molecular absorption are shown to be consistent with high-quality observed profiles for the giants γ Tau (K0), μ Leo (K2) and μ Peg (G8). The magnesium abundances and overall metallicities indicated by this comparison are respectively +0.15, +0.4 and -0.1, in logarithmic units relative to the Sun.

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