The European Physical Journal A

, Volume 36, Issue 2, pp 233–241 | Cite as

The definition of the effective interaction energy for astrophysical relevant reactions

Special Article - Tools for Experiment and Theory

Abstract.

Experimental studies of nuclear reactions of astrophysical interest are hampered by the exponential drop of the cross-section with decreasing energy. Generally, the effects of the projectile energy loss in the target cannot be neglected and the reaction yield is proportional to the average value of the cross-section over the interaction energies inside the target. Local cross-section values, instead of averaged, are needed to evaluate stellar reaction rates. To deal with this, several different effective interaction energy definitions have been introduced during the years, leading to potentially discrepant results. Thus, a well-defined procedure for data reduction is required. This work briefly reviews the theoretical ground for the experimental cross-section data reduction and the effective interaction energies definitions up to now introduced. The self-consistent approach introduced by B.W. Filippone et al. is discussed and its application to the data analysis of non-resonant and narrow-resonant reactions is presented. A comparison of the results obtained using the different approaches is also reported.

PACS.

29.85.-c Computer data analysis 24.50.+g Direct reactions 24.30.-v Resonance reactions 

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References

  1. 1.
    C. Rolfs, W.S. Rodney, Cauldrons in the Cosmos (University of Chicago Press, Chicago, 1988).Google Scholar
  2. 2.
    C. Angulo, Nucl. Phys. A 656, 3 (1999).CrossRefADSMathSciNetGoogle Scholar
  3. 3.
    C. Arpesella, Nucl. Instrum. Methods Phys. Res. A 360, 607 (1995).CrossRefADSGoogle Scholar
  4. 4.
    P.R. Wrean, C.R. Brune, R.W. Kavanagh, Phys. Rev. C 49, 1205 (1994).CrossRefADSGoogle Scholar
  5. 5.
    B.W. Filippone, Phys. Rev. C 28, 2222 (1983).CrossRefADSGoogle Scholar
  6. 6.
    W.H. Press, S.A. Teukolsky, W.T. Vetterling, B.P. Flannery, Numerical Recipes in C: The Art of Scientific Computing, second edition (Cambridge University Press, 1992).Google Scholar
  7. 7.
    A. Lemut, unpublished.Google Scholar
  8. 8.
    C. Casella, Nucl. Phys. A 706, 203 (2002).CrossRefADSGoogle Scholar
  9. 9.
    H.H. Andersen, J.F. Ziegler, Stopping Powers and Ranges in All Elements (Pergamon Press, 1977) (updated data are available on-line at http://www.srim.org).Google Scholar
  10. 10.
    H.J. Assenbaum, K. Langanke, C. Rolfs, Z. Phys. A 327, 461 (1987).Google Scholar
  11. 11.
    G. Imbriani, Eur. Phys. J. A 25, 455 (2005).CrossRefADSGoogle Scholar
  12. 12.
    C. Iliadis, Nuclear Physics of Stars (Physics Textbook, WILEY-VCH Verlag GmbH & Co. KgaA, Weinheim, 2007).Google Scholar

Copyright information

© Società Italiana di Fisica and Springer-Verlag 2008

Authors and Affiliations

  1. 1.Istituto Nazionale di Fisica Nucleare Sezione di GenovaGenovaItaly

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