EAS Publications Series

Issue		EAS Publications Series Volume 11, 2004 The Future Astronuclear Physics
Page(s)		217 - 225
DOI		10.1051/eas:2004015

The Future Astronuclear Physics
A. Jorissen, S. Goriely, M. Rayet, L. Siess and H. Boffin (eds)
EAS Publications Series, Vol. 11, 2004
DOI: 10.1051/eas:2004015

Some ideas concerning the future of Nuclear Astrophysics illustrated by the example of the key reaction $\mathsf}$ C( $\alpha,\gamma$ ) $\mathsf}$ O

J.W. Hammer

Institut für Strahlenphysik, University of Stuttgart, Allmandring 3, 70569 Stuttgart, Germany

Abstract
The key reaction ¹²C( $\alpha,\gamma$ ) ¹⁶O is taken as example and illustration for research on extremely slow and complicated reactions of astrophysical interest. Two sensitive experiments in the energy range $E_{\rm c.m.} = 890{-}2800$ keV have been performed and the extrapolation to 300 keV of the S-factors obtained by an R-matrix analysis are $S_{\rm E1}^$ = (77 $\pm$ 17) keV b; $S_{\rm E2}^$ = (81 $\pm$ 22) keV b; $S_{\rm tot}^$ = (162 $\pm$ 40) keV b. The astrophysical reaction rate has been determined with $\pm$ 25% precision in the temperature range 0.001 $\leq$ T₉ $\leq$ 10. From 30 years of research on this reaction, some problems related to experimental nuclear astrophysics become evident and suggestions for improving future works are made.

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Some ideas concerning the future of Nuclear Astrophysics illustrated by the example of the key reaction C( ) O

Some ideas concerning the future of Nuclear Astrophysics illustrated by the example of the key reaction $\mathsf}$ C( $\alpha,\gamma$ ) $\mathsf}$ O