The ν process in the innermost supernova ejecta

¹ Institute for Nuclear Physics (Theory Department), Darmstadt University of Technology, Schlossgartenstraße 2, 64289 Darmstadt, Germany
² Helmholtz Center for Heavy Ion Research (GSI), Planckstr. 1, 64259 Darmstadt, Germany
³ Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
⁴ Physics Division, Oak Ridge National Laboratory, P.O. Box 2008, Oak Ridge, TN 37831-6354, USA
⁵ Department of Physics and Astronomy, University of Tennessee, Knoxville, TN 37996-1200, USA

^* e-mail: asiever@theorie.ikp.physik.tu-darmstadt.de

Published online: 30 December 2017

Abstract

The neutrino-induced nucleosynthesis (ν process) in supernova explosions of massive stars of solar metallicity with initial main sequence masses between 13 and 30 M_⊙ has been studied with an analytic explosion model using a new extensive set of neutrino-nucleus cross-sections and spectral properties that agree with modern supernova simulations. The production factors for the nuclei ⁷Li, ¹¹B, ¹⁹F, ¹³⁸La and ¹⁸⁰Ta, are still significantly enhanced but do not reproduce the full solar abundances. We study the possible contribution of the innermost supernova eject to the production of the light elements ⁷Li and ¹¹B with tracer particles based on a 2D supernova simulation of a 12 M_⊙ progenitor and conclude, that a contribution exists but is negligible for the total yield for this explosion model.