Transition probabilities in TI I and the solar titanium abundance

Details Transition probabilities in TI I and the solar titanium abundance Transition probabilities in TI I and the solar titanium abundance

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...212..581w&link_type=abstract

Astrophysical Journal, Part 1, vol. 212, Mar. 1, 1977, p. 581-590.

Mathematics

40

Abundance, Line Spectra, Meteoritic Composition, Solar Spectra, Titanium, Transition Probabilities, Atomic Spectra, Branching (Mathematics), Photosphere, Radiative Lifetime, Spectral Line Width, Spectrum Analysis, Tables (Data)

Scientific paper

Branching ratios have been measured for 103 lines from 14 levels in Ti I, and absolute transition probabilities have been determined by combining these branching ratios with the radiative lifetimes measured by Roberts, Sorensen, and Andersen (1973) by the beam-foil method. The solar equivalent width at the disk center has been measured for 23 of these lines on the preliminary edition of the Kitt Peak Solar Atlas. The solar Ti abundance has been computed by matching the equivalent widths of 15 of the weakest lines and by fitting the profiles of 16 lines. The two methods yield an average photospheric abundance log (N(Ti)/N(H)) + 12 = 4.98 plus or minus 0.15 based on the HSRA solar model.

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