Determination of alpha spectroscopic factors for unbound 17O states
1 Institut de Physique Nucléaire d’Orsay, UMR8608, IN2P3-CNRS, Université Paris sud 11, 91406 Orsay, France
2 Department of Physics, University of York, York YO10 5DD, United Kingdom
3 E. A. Milne Centre for Astrophysics, Deparment of Physics and Mathematics, University of Hull, HU6 7RX, United Kingdom
* e-mail: e-mail: firstname.lastname@example.org
Published online: 30 December 2017
It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could lead to high 13C and 15N excesses when the blast of a core collapse supernova (ccSN) passes through its helium shell. This prediction questions the origin of extremely high 13C and 15N abundances observed in rare presolar SiC grains which is usually attributed to classical novae. In this context the 13N(α,p)16O reaction plays an important role since it is in competition with 13N β+-decay to 13C. As a first step to the determination of the 13N(α,p)16O reaction rate, we present a study aiming at the determination of alpha spectroscopic factors of 17O states which are the analog ones to those in 17F, the compound nucleus of the 13N(α,p)16O reaction.
© 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/).