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Reduction of deuterium content in carbon targets for 12C + 12C reaction studies of astrophysical interest

  • L. Morales-Gallegos
  • M. Aliotta
  • C. G. Bruno
  • R. Buompane
  • T. Davinson
  • M. De Cesare
  • A. Di Leva
  • A. D’Onofrio
  • J. G. Duarte
  • L. R. Gasques
  • L. Gialanella
  • G. Imbriani
  • G. Porzio
  • D. Rapagnani
  • M. Romoli
  • D. Schürmann
  • F. Terrasi
  • L. Y. Zhang
Open Access
Regular Article - Experimental Physics
  • 14 Downloads

Abstract.

The 12C(12C,p)23Na and 12C(12C,\(\alpha\))20Ne fusion reactions are among the most important in stellar evolution since they determine the destiny of massive (\( M \simeq 8-10 M_{\odot}\)) stars. However, experimental low-energy investigations of such reactions are significantly hampered by ubiquitous natural hydrogen and deuterium contaminants in the carbon targets. The associated beam-induced background completely masks the reaction products of interest thus preventing cross-section measurements at the relevant energies of astrophysical interest, \(E_{\mathrm{cm}} < 2\) MeV. In this work, we report about an investigation aimed at assessing possible deuterium reductions on both natural graphite and Highly Ordered Pyrolytic Graphite targets as a function of target temperature. Our results indicate that reductions up to about 80% can be attained on both targets in the temperature range investigated, \( T \simeq 200-1200 {}^{\circ}\)C. A further reduction by a factor of 2.5 in absolute deuterium content is observed when the scattering chamber is surrounded by a dry nitrogen atmosphere so as to minimise light-particles uptake within the chamber rest gas (and thus on target) through air leaks. The results from this study will inform the choice of optimal experimental conditions and procedures for improved measurements of the 12C + 12C reactions cross-sections at the low energies of astrophysical interest.

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Copyright information

© The Author(s) 2018

Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Authors and Affiliations

  • L. Morales-Gallegos
    • 1
    • 2
  • M. Aliotta
    • 1
    • 3
  • C. G. Bruno
    • 1
  • R. Buompane
    • 3
    • 2
  • T. Davinson
    • 1
  • M. De Cesare
    • 4
    • 2
  • A. Di Leva
    • 5
    • 2
  • A. D’Onofrio
    • 3
    • 2
  • J. G. Duarte
    • 3
    • 2
  • L. R. Gasques
    • 6
    • 3
    • 2
  • L. Gialanella
    • 3
    • 2
  • G. Imbriani
    • 5
    • 2
  • G. Porzio
    • 3
  • D. Rapagnani
    • 7
    • 8
  • M. Romoli
    • 2
  • D. Schürmann
    • 3
    • 2
  • F. Terrasi
    • 3
    • 2
  • L. Y. Zhang
    • 9
    • 1
  1. 1.SUPA, School of Physics and AstronomyUniversity of EdinburghEdinburghUK
  2. 2.INFN, Sezione di NapoliNapoliItaly
  3. 3.Dipartimento di Matematica e FisicaUniversità degli Studi della Campania “Luigi Vanvitelli”CasertaItaly
  4. 4.Centro Italiano di Ricerche AerospazialiCapuaItaly
  5. 5.Dipartimento di Fisica “E. Pancini”Università degli Studi di Napoli “Federico II”NapoliItaly
  6. 6.Departamento de Física NuclearInstituto de Física da Universidade de São PauloSão PauloBrazil
  7. 7.Dipartimento di Fisica e GeologiaUniversità degli Studi di PerugiaPerugiaItaly
  8. 8.INFN, Sezione di PerugiaPerugiaItaly
  9. 9.National Astronomical ObservatoriesChinese Academy of SciencesLanzhouChina

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