Abstract
Oscillator strengths are calculated for 259 lines of Ti i by taking configuration interaction into account in a somewhat simplified treatment. Radial integrals are obtained by an adaptation of the scaled Thomas-Fermi method. The great majority of selected lines originate from slightly perturbed terms. From a satisfactory comparison of our g \({\text{f}}\) -values with recent experimental data and with solar results in the visible region, we have been able to extend the work for some infrared lines. Very few transition probabilities were known for Ti i in that spectral range.
On the basis of our oscillator strengths, a mean value logN ti = 4.88 ± 0.12 (in the usual scale), is proposed for the solar photospheric abundance, in agreement with the meteoritic value.
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Allen, C. W.: 1934, Mémoir No. 5, Part 2, Commonwealth Solar Physics Observatory (quoted by Tatum, J. B.: 1961).
Allen, C. W.: 1960, Monthly Notices Roy. Astron. Soc. 121, 299.
Allen, C. W.: 1973, Astrophysical Quantities, 3rd ed., The Athlone Press, London.
Aller, L. H.: 1968, Proc. Astron. Soc. Australia 1, 133.
Bates, D. R. and Damgaard, A.: 1949, Phil. Trans. Roy. Soc. London 242, 101.
Boyarchuk, M. E. and Boyarchuk, A. A.: 1960, Izv. Krymsk. Astrofiz. Obs. 22, 234.
Cameron, A. G. W.: 1968, in L. H. Ahrens (ed.), The Origin and Distribution of the Elements, Pergamon Press.
Cameron, A. G. W.: 1973, Space Sci. Rev. 15, 121.
Cooper, J. and Palmer, U.: 1967, JILA Report No. 91, Boulder, Colorado.
Corliss, C. H. and Bozman, W. R.: 1962, NBS Monograph, No. 53.
Delbouille, L., Neven, L., and Roland, G.: 1973, Atlas photométrique du spectre solaire de λ3000 à λ10000 Å, Institut d'Astrophysique de l'Université de Liège.
Dosinas, G., Vizbaraite, J., Rudzikas, Z., and Jucys, A.: 1968, Lietuvos Fizikos Rinkinys 8, 53.
Froese Fisher, C.: 1968, Astrophys. J. 151, 759.
Froese Fischer, C.: 1973, J. Quant. Spectr. Radiat. Transfer 13, 201.
Gingerich, O., Noyes, R. W., Kalkofen, W., and Cuny, Y.: 1971, Solar Phys. 18, 347.
Goldberg, L., Müller, E. A., and Aller, L. H.: 1960, Astrophys. J. Suppl. 5, 1.
Grevesse, N.: 1969, Ph. D. Thesis, University of Liège.
Hefferlin, R., Cobb, B., Hall, D., and Lehman, C.: 1960, Astrophys. J. 132, 259.
Kandel, R.: 1960, Ann. Astrophys. 23, 995.
Kiess, C. C. and Thekaekara, M. P.: 1959, Astrophys. J. 87, 24.
King, R. B. and King, A. S.: 1938, Astrophys. J. 87, 24.
Klemt, M.: 1973, Astron. Astrophys. 29, 419.
Mitrofanova, L. A.: 1955, Pulkovo Astron. Obs. Izvest. 19, 107.
Moore, C. E.: 1949, ‘Atomic Energy Levels’, NBS Circular, No. 467, Vol. 1.
Moore, C. E.: 1959, ‘A Multiplet Table of Astrophysical Interest’, NBS Technical Note, No. 36.
Moore, C. E., Minnaert, M. G. J., and Houtgast, J.: 1966, ‘The Solar Spectrum 2935 Å to 8770 Å’, NBS Monograph 61.
Morozova, N. P. and Startsev, G. P.: 1964, Opt. Spectrosc. 17, 174.
Müller, E. A.: 1968, in L. H. Ahrens (ed.), Origin and Distribution of the Elements, Pergamon Press.
Müller, E. A. and Mutschlecner, J. P.: 1964, Astrophys. J. Suppl. 9, 1.
Prokofiev, V. K. and Ratobylskaya, T. A.: 1969, Izv. Krymsk. Astrofiz. Obs. 39, 186.
Reinke, P.: 1967, Z. Astrophys. 66, 234.
Roberts, J. R., Andersen, T. and Sorensen, G.: 1973, Astrophys. J. 181, 567.
Rohrlich, F.: 1948, Phys. Rev. 74, 1381.
Roth, C.: 1969, J. Res. Nat. Bur. Stand. 73A, 497.
Russel, H. N.: 1929, Astrophys. J. 70, 11.
Shackleford, W. L.: 1962, J. Quant. Spectr. Radiat. Transfer 2, 245.
Shore, B. W. and Menzel, D. H.: 1965, Astrophys. J. Suppl. 12, 187.
Smith, M. W. and Wiese, W. L.: 1971, Astrophys. J. Suppl. 23, 103.
Stewart, J. C. and Rotenberg, M.: 1965, Phys. Rev. 140, 1508.
Takens, R. J.: 1970, Astron. Astrophys. 5, 244.
Tatum, J. B.: 1961a, Monthly Notices Roy. Astron. Soc. 122, 311.
Tatum, J. B.: 1961b, Communications from the University of London Observatory, No. 41.
Teplitskaya, R. B. and Vorobeva, V. A.: 1964, Soviet Astron. 7, 778.
Thekaekara, M. P.: 1959, Georgetown Observatory Monograph, No. 13.
Unsöld, A.: 1948, Z. Astrophys. 24, 306.
Unsöld, A.: 1955, Physik der Sternatmosphären, 2nd ed., Springer Verlag.
Urey, H. C.: 1967, Quart, J. Roy. Astron. Soc. 8, 23.
Van Stekelenburg, L. H. M. and Smit, J. A.: 1948, Physica 14, 189.
Vizbaraite, J., Rudzikas, Z., and Grabauskas, D.: 1968, Lietuvos Fizikos Rinkinys 8, 481.
Warner, B.: 1968a, Montly Notices Roy. Astron. Soc. 138, 229.
Warner, B.: 1968b, Monthly Notices Roy. Astron. Soc. 139, 1.
Wilson, C. M. and Thekaekara, M. P.: 1961, J. Opt. Soc. Am. 51, 289.
Withbroe, G. L.: 1971, in ‘The Menzel Symposium on Solar Physics, Atomic Spectra and Gazeous Nebulae’, NBS special publication, No. 353.
Wolnik, S. J. and Berthel, R. O.: 1973, Astrophys. J. 179, 665.
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Biémont, E. Computation of oscillator strengths by a semi-empirical method for some elements of the iron-group and their solar photospheric abundance. Sol Phys 38, 15–31 (1974). https://doi.org/10.1007/BF00161820
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DOI: https://doi.org/10.1007/BF00161820