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 

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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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