EPJ Web Conf.
Volume 163, 2017FUSION17
|Number of page(s)||4|
|Published online||22 November 2017|
How well do we understand the reaction rate of C burning?
IPHC, Université de Strasbourg, F-67037 Strasbourg, France
2 CNRS, UMR7178, F-67037 Strasbourg, France
3 USIAS, F-67083 Strasbourg, France
4 Physics Division, Argonne National Laboratory, Argonne, IL 60439, USA
5 Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA70803, USA
6 Department of Physics, University of York, Heslington, York YO10 5DD, UK
7 CSNSM IN2P3-CNRS and University of Paris Sud, F-91405 Orsay, France
8 Department of Physics, Florida State University, Tallahassee, FL 32306, USA
9 University of Notre Dame, Notre Dame, IN 46556, USA
10 Institute of Modern Physics, Lanzhou, China
11 TRIUMF, Vancouver, BC V6T 2A3, Canada
12 Lawrence Livermore National laboratory, Livermore, CA 94551, USA
* e-mail: firstname.lastname@example.org
Published online: 22 November 2017
Carbon burning plays a crucial role in stellar evolution, where this reaction is an important route for the production of heavier elements. A particle-γ coincidence technique that minimizes the backgrounds to which this reaction is subject and provides reliable cross sections has been used at the Argonne National Laboratory to measure fusion cross-sections at deep sub-barrier energies in the 12C+12C system. The corresponding excitation function has been extracted down to a cross section of about 6 nb. This indicates the existence of a broad S-factor maximum for this system. Experimental results are presented and discussed.
© The Authors, published by EDP Sciences, 2017
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (http://creativecommons.org/licenses/by/4.0/).
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