• Open Access

Stellar and thermal neutron capture cross section of Be9

A. Wallner, M. Bichler, L. Coquard, I. Dillmann, O. Forstner, R. Golser, M. Heil, F. Käppeler, W. Kutschera, C. Lederer-Woods, M. Martschini, A. Mengoni, S. Merchel, L. Michlmayr, A. Priller, P. Steier, and M. Wiescher
Phys. Rev. C 99, 015804 – Published 14 January 2019

Abstract

The neutron capture cross section of Be9 for stellar energies was measured via the activation technique using the Karlsruhe Van de Graaff accelerator in combination with accelerator mass spectrometry at the Vienna Environmental Research Accelerator. To characterize the energy region of interest for astrophysical applications, activations were performed in a quasistellar neutron spectrum of kT=25 keV and for a spectrum at En=473±53 keV. Despite the very small cross section, the method used provided the required sensitivity for obtaining fairly accurate results of 10.4±0.6 and 8.4±1.0μb, respectively. With these data it was possible to constrain the cross section shape up to the first resonances at 622 and 812 keV, thus allowing for the determination of Maxwellian-averaged cross sections at thermal energies between kT=5 and 100 keV. In addition, we report a new experimental cross section value at thermal energy of σth=8.31±0.52 mb.

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  • Received 21 August 2018
  • Revised 22 October 2018
  • Corrected 30 May 2019

DOI:https://doi.org/10.1103/PhysRevC.99.015804

Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.

Published by the American Physical Society

Physics Subject Headings (PhySH)

Nuclear PhysicsAccelerators & BeamsGravitation, Cosmology & Astrophysics

Corrections

30 May 2019

Correction: The ordinate axis label in Fig. 1 contained an error and has been fixed. Some entries in Tables 10 and 11 needed adjustment and have been resolved.

Authors & Affiliations

A. Wallner1,2,*, M. Bichler3, L. Coquard4, I. Dillmann4,†, O. Forstner2,‡, R. Golser2, M. Heil4,§, F. Käppeler4, W. Kutschera2, C. Lederer-Woods5, M. Martschini2, A. Mengoni6, S. Merchel7, L. Michlmayr2, A. Priller2, P. Steier2, and M. Wiescher8

  • 1Department of Nuclear Physics, Research School of Physics and Engineering, The Australian National University, Canberra, ACT 2601, Australia
  • 2VERA Laboratory, Faculty of Physics, University of Vienna, Austria
  • 3Atominstitut, Vienna University of Technology, Austria
  • 4Karlsruhe Institute of Technology (KIT), Campus North, Institute of Nuclear Physics, PO Box 3640, Karlsruhe, Germany
  • 5School of Physics and Astronomy, University of Edinburgh, United Kingdom
  • 6CERN, CH-1211 Geneva 23, Switzerland
  • 7Helmholtz-Zentrum Dresden-Rossendorf, Helmholtz Institute Freiberg for Resource Technology, 01328 Dresden, Germany
  • 8Department of Physics and Joint Institute of Nuclear Astrophysics, University of Notre Dame, Notre Dame, Indiana, USA

  • *anton.wallner@anu.edu.au
  • Present address: TRIUMF, Vancouver BC, Canada.
  • Present address: Friedrich-Schiller-Universität Jena and Helmholtz-Institut Jena, 07743 Jena, Germany and GSI Helmholtzzentrum für Schwerionenforschung, 64291 Darmstadt, Germany.
  • §Present address: GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany.

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Issue

Vol. 99, Iss. 1 — January 2019

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