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Solar Physics

, Volume 23, Issue 1, pp 13–17 | Cite as

The solar abundance of gold

  • John E. Ross
  • Lawrence H. Aller
Article

Abstract

From 13 scans obtained with a double-band pass spectrograph at the Snow telescope at Mount Wilson, interpreted by the method of spectral synthesis, the abundance of gold turns out to be log [N(Au)/N(H)] + 12 = 0.70, assuming loggf = − 0.57.

Keywords

Gold Spectral Synthesis Solar Abundance 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. Aller, L. H.: 1968, Trans. Astron. Soc. Australia 1.Google Scholar
  2. Corliss, C. H. and Bozman, W. R.: 1962, Experimental Transition Probabilities for Spectral Lines of Seventy Elements, N.B.S. Mono. Nr. 53, Washington, D.C., U.S. Government printing office.Google Scholar
  3. Grevesse, N., Blanquet, G., and Boury, A.: 1967, Paris Symposium on Abundance of Elements.Google Scholar
  4. Lawrence, G. M., Link, J. K., and King, R. B.: 1965, Astrophys. J. 141, 293.Google Scholar
  5. Moise, N. L.: 1966, Astrophys. J. 144, 774.Google Scholar
  6. Penkin, N. P. and Slavenas, L.-Yu.: 1963, Opt. Spectrosc. 15, 3.Google Scholar
  7. Ross, John E.: 1971, quoted in Aller, L. H., Atoms, Stars and Nebulae, Harvard University Press, Cambridge.Google Scholar

Copyright information

© D. Reidel Publishing Company 1972

Authors and Affiliations

  • John E. Ross
    • 1
  • Lawrence H. Aller
    • 1
  1. 1.University of CaliforniaLos AngelesU.S.A.

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