Supersymmetric Grand Unification

  • Rabindra N. Mohapatra
Part of the Graduate Texts in Contemporary Physics book series (GTCP)


One of the original motivations for the application of supersymmetry to particle physics was to solve the gauge hierarchy problem that arises in the grand unification program. As has been emphasized in Chapter 5, the tree level parameters must be fine tuned to an accuracy of 10-26 or so, to generate the mass ratio M x /m w ≃ 1012 in the SU(5) model. In other models, due to the presence to intermediate mass scales, the problem of fine tuning is not as severe but a lesser degree of fine tuning is always required. Since a nonsupersymmetric theory with scalar bosons is plagued with quadratic divergences, such tree level fine tunings are upset in higher orders. This need not happen in supersymmetric theories due to the nonrenormalization theorem of Grisaru, Rocek, and Siegel described in Chapter 10. According to this theorem, the parameters of the superpotentials do not only receive infinite renormalization but they also do not receive finite renormalization in higher orders. Supersymmetry can, therefore, be used to solve one aspect of the gauge hierarchy problem, i.e., once we fine tune parameters at the tree level the radiative corrections do not disturb the hierarchy. This point was utilized by Dimopoulos and Georgi [1] and Sakai [2] to construct supersymmetric SU(5) models with partial solutions to the gauge hierarchy problem. We illustrate their procedure with a simple but realistic supersymmetric SU(5) model.


Radiative Correction Proton Decay Higgs Field Nonrenormalization Theorem Grand Unification 
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]
    S. Dimopoulos and H. Georgi, Nucl. Phys. B193, 150 (1981).Google Scholar
  2. [2]
    N. Sakai, Z. Phys. C11, 153 (1981).Google Scholar
  3. [3]
    S. Weinberg, Phys. Rev. D25, 287 (1982);CrossRefGoogle Scholar
  4. N. Sakai and T. Yanagida, Nucl. Phys. B197, 533 (1982).ADSCrossRefGoogle Scholar
  5. [4]
    M. B. Einhorn and D. R. T. Jones, Nucl. Phys. 13196, 475 (1982);ADSCrossRefGoogle Scholar
  6. W. Marciano and G. Senjanovic, Phys. Rev D25, 3092 (1982).Google Scholar
  7. [5]
    J. Ellis, D. V. Nanopoulos, and S. Rudaz, Nucl. Phys. B202, 43 (1982); For a recent analysis see J. Milutinovich; P. Pal, and G. Senjanovic, ITP Santa Barbara preprint, 1984.Google Scholar
  8. [6]
    E. Witten, Phys. Lett. 105B, 267 (1981).Google Scholar
  9. [7]
    S. Coleman and E. Weinberg, Phys. Rev. D7, 1888 (1973).Google Scholar
  10. [8]
    H. Yamagishi, Nucl. Phys. B216, 508 (1983);ADSCrossRefGoogle Scholar
  11. L. Hall and I. Hinchliffe, Phys. Lett 119B, 128 (1982).Google Scholar
  12. [9]
    S. Dimopoulos and S. Raby, Nucl. Phys. B219, 479 (1983).Google Scholar
  13. [10]
    S. Kalara and R. N. Mohapatra, Phys. Rev. D28, 2241 (1983).Google Scholar
  14. [11]
    B. Ovrut and S. Raby, Phys. Lett. 125B, 270 (1983).Google Scholar

Copyright information

© Springer Science+Business Media New York 1992

Authors and Affiliations

  • Rabindra N. Mohapatra
    • 1
  1. 1.Department of Physics and AstronomyUniversity of MarylandCollege ParkUSA

Personalised recommendations