Measurement of relative oscillator strengths for TI I. III Weak transitions from levels a3F(3, 4) (0.02 eV, 0.05 eV), a5F(1-5) (0.81 eV-0.85 eV), a1D(2) (0.90 eV), a3P(0-3) (1.05 eV-1.07 eV) with solar analysis

Details Measurement of relative oscillator strengths for TI I. III Weak transitions from levels a3F(3, 4) (0.02 eV, 0.05 eV), a5F(1-5) (0.81 eV-0.85 eV), a1D(2) (0.90 eV), a3P(0-3) (1.05 eV-1.07 eV) with solar analysis Measurement of relative oscillator strengths for TI I. III Weak transitions from levels a3F(3, 4) (0.02 eV, 0.05 eV), a5F(1-5) (0.81 eV-0.85 eV), a1D(2) (0.90 eV), a3P(0-3) (1.05 eV-1.07 eV) with solar analysis

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.204..883b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 204, Sept. 1983, p. 883-890. Research supported by the

Astronomy and Astrophysics

Astronomy

48

Fluorine, Line Spectra, Oscillator Strengths, Solar Spectra, Spectrum Analysis, Titanium, Solar Temperature, Stellar Temperature

Scientific paper

The relative oscillator strengths presently given for 18 weak 1-eV and two 0-eV lines of Ti I have been measured with a relative accuracy of 5 percent by means of the Oxford furnace technique. Relative values are placed on the absolute scale previously derived for stronger 0- and 1-eV lines, and a solar analysis is made for the most suitable lines as a test of their oscillator strengths. Although this is not regarded as a definitive solar analysis, because of the weakness of the solar lines, the value of log A = 5.08, with a microturbulence value of 0.89 km/sec, both agree well with those already found for stronger 0-eV lines.

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Measurement of relative oscillator strengths for TI I. III Weak transitions from levels a3F(3, 4) (0.02 eV, 0.05 eV), a5F(1-5) (0.81 eV-0.85 eV), a1D(2) (0.90 eV), a3P(0-3) (1.05 eV-1.07 eV) with solar analysis does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

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