Solar Neutrinos: Theory

  • J. N. Bahcall
Conference paper


The solar neutrino problem can be stated simply. The observed capture rate is [1,2]:
$$ Observed = \left( {2\pm 0.3} \right)SNU $$
The predicted capture rate for the 37Cl experiment is [3,4]:
$$ \Pr edicted = \left( {7.5\pm 2.5} \right)SNU $$
[The convenient unit for discussing solar neutrinos is the product of a flux times a cross section and is: 1 SNU = 10-36 events per target particle per second. I give here preliminary values of event rates predicted by the standard solar model that have been obtained by an improved set of calculations with updated parameters. The final values will be published in reference 4.] The observational error quoted above is 1-σ(by tradition); the error I quote on the predicted rate corresponds to an effective 3-σ auncertainty, defined in [3]. The fact that the theoretical and the experimental numbers differ significantly is the solar neutrino problem. There is no generally accepted solution to the problem although neutrino oscillations in matter provides a plausible and attractive hypothesis [5,6].


Neutrino Oscillation Solar Neutrino Stellar Evolution Neutrino Flux Neutrino Spectrum 
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.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. 1.
    R. Davis, in Proceedings Informal Conference on Status and Future of Solar Neutrino Research edited by G. Friedlander (BNL Report 40879, 1978), Vol. 1, p. 1.Google Scholar
  2. 2.
    J.N. Bahcall, B. T. Cleveland, R. Davis, Jr., and J. K. Roweley, Ap. J. Letters 292, L79–L82 (1985).ADSCrossRefGoogle Scholar
  3. 3.
    J.N. Bahcall, W.R. Huebner, S.H. Lubow, P.D. Parker, and R.K. Ulrich, Rev. Mod. Phys., 54, 767 (1982).ADSCrossRefGoogle Scholar
  4. 4.
    J. N. Bahcall and R. K. Ulrich (in preparation) (1986).Google Scholar
  5. 5.
    S.P. Mikheyev and A. Yu. Smirnov, 10th International Workshop, Savonlinna, Finland, June 16–25, 1985Google Scholar
  6. 5a.
    L. Wolfenstein, Phys. Rev. D20, 2634 (1979).Google Scholar
  7. 6.
    S. P. Rosen and J. M. Gelb, Phys. Rev. D (submitted) (1986)Google Scholar
  8. 6.
    H. A. Bethe, Phys. Rev. Letters 56, 1305 (1986).ADSCrossRefGoogle Scholar
  9. 7.
    P. D. Parker, in Physics of the Sun, Vol. 1, p. 15 (D. Reidel, New York, 1986).Google Scholar
  10. 8.
    S. J. Freedman, Argonne preprint PHY=4682 (1986).Google Scholar
  11. 9.
    J. N. Bahcall and B. Holstein, Phys. Rev. C, 33, 2121 (1986).ADSCrossRefGoogle Scholar
  12. 10.
    F. C. Barker and R. H. Spear, Ap. J. (to be published) (1986).Google Scholar
  13. 11.
    G. A. Cowan and W. C. Haxton, Science 216,51 (1982).ADSCrossRefGoogle Scholar
  14. 12.
    G. A. Cowan, private communication (1986).Google Scholar
  15. 13.
    J. N. Bahcall, Phys. Rev.C, 24, 2216 (1981).ADSCrossRefGoogle Scholar
  16. 14.
    G. S. Hurst et al., Phys. Rev. Letters 53, 1116(1984).ADSCrossRefGoogle Scholar
  17. 15.
    J. N. Bahcall, M. Baldo-Ceollin, D. Cline, and C. Rubbia, Phys. Letters (submitted) (1986).Google Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 1986

Authors and Affiliations

  • J. N. Bahcall
    • 1
  1. 1.Institute for Advanced StudyPrincetonUSA

Personalised recommendations