atomic data, sun, abundances
Transition probabilities of 100 Ti-II emission lines, originating from 7 different atomic levels, have been determined by combining branching fractions with radiative lifetimes. The branching fractions were meaures using Fourier transform spectroscopy on a hollow cathode. The radiative lifetimes of these 7 – and 35 additional – levels were measured using time resolved laser-induced fluorescence on a slow Ti ion beam. The transition probabilities of 21 very weak lines have been used to derive a solar titanium abundance of aTi=log(NTi/NH)+12=5.04±0.04 dex, which is insensitive to the solar model. This value is in disagreement with the meteoritic titanium abundance (4.93 ± 0.02).
Original Publication Citation
A. Bizzarri, M. C. E. Huber, A. Noels, N. Grevesse, S. D. Bergeson, P. Tsekeris, and J. E. Lawler. Ti-ii transition probabilities and radiative lifetimes in TI and the solar titanium abundance. Astron. Astrophys. 273 (2), 707-718 (1993).
BYU ScholarsArchive Citation
Bizzarri, A.; Huber, M.C.E.; Noels, A.; Grevesse, N.; Bergeson, Scott D.; Tsekeris, P.; and Lawler, J. E., "Ti-II Transition Probabilities and Radiative Lifetimes in Ti+ and the Solar Titanium Abundance" (1993). Faculty Publications. 1825.
American Astronomical Society
Physical and Mathematical Sciences
Physics and Astronomy
© 1993 American Astronomical Society. This article is the Version of Record published by the American Astronomical Society in Astrophysical Journal in 1993 , available online at http://adsabs.harvard.edu/full/1993A%26A...273..707B
Copyright Use Information