Abstract
16 lines of Pr ii possibly present in the solar photospheric spectrum have been studied. When including hyperfine structure in synthetic calculations, investigations of 9 lines result in an abundance A Pr = 0.71 ± 0.08 in the log A H = 12.00 scale.
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Andersen, T., Poulsen, C., Ramanujam, P. S., and Petkov, A. P.: 1975, Solar Phys. 44, 257.
Biémont, E.: 1978, Solar Phys. 56, 79.
Blaise, J.: 1978, private communication.
Brault, J. and Testerman, L.: 1972, Preliminary Edition of the Kitt Peak Solar Atlas, unpublished.
Cameron, A. G. W.: 1973, Space Sci. Rev. 15, 121.
Candler, C.: 1964, Atomic Spectra, Hilger and Watts Ltd., London.
Corliss, C. H. and Bozman, W. R.: 1962, Nat. Bur. Std. Monograph No. 53.
Delbouille, L., Neven, L., and Roland, G.: 1973, Atlas Photométrique du Spectre Solaire de λ3000 à λ10 000, Institute of Astrophysics, University of Liège.
Grevesse, N. and Blanquet, G.: 1969, Solar Phys. 8, 5.
Holweger, H. and Müller, E. A.: 1974, Solar Phys. 39, 19.
Lage, C. S. and Whaling, W.: 1976, J. Quant. Spectr. Radiat. Transfer 16, 537.
Moore, C. E., Minnaert, M. G. J., and Houtgast, J.: 1966, Nat. Bur. Std. Monograph No. 61.
Righini, A. and Rigutti, M.: 1966, Ann. Astrophys. 29, 379.
Shore, B. W. and Menzel, D. H.: 1965, Astrophys. J. Suppl. 12, 187.
Rosen, N., Harison, G. R., and McNally, J. R.: 1941, Phys. Rev. 60, 722.
White, H. E.: 1929, Phys. Rev. 34, 1397.
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Biémont, E., Grevesse, N. & Hauge, Ø. Solar abundance of praseodymium. Sol Phys 61, 17–22 (1979). https://doi.org/10.1007/BF00155442
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DOI: https://doi.org/10.1007/BF00155442