Eur. Phys. J. A (2020) 56: 108
https://doi.org/10.1140/epja/s10050-020-00106-y

Regular Article – Experimental Physics

Spin assignments for levels and the astrophysical reaction

¹ Department of Physics, Sungkyunkwan University, Suwon, 16149, South Korea
² Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee, 37996, USA
³ Department of Physics, University of Notre Dame, Notre Dame, IN, 46556, USA
⁴ Department of Physics, Colorado School of Mines, Golden, CO, 80401, USA
⁵ Department of Physics and Astronomy, Rutgers University, New Brunswick, NJ, 08903, USA
⁶ Department of Physics, Tennessee Technological University, Cookeville, TN, 38505, USA
⁷ Department of Physics, School of Natural Science, Ulsan National Institute of Science and Technology (UNIST), Ulsan, 44919, South Korea
⁸ Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA, 70803, USA
⁹ Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN, 37831, USA
¹⁰ Oak Ridge Associated Universities, Oak Ridge, TN, 37831, USA

^* e-mail: kchae@skku.edu

Received: 20 October 2019
Accepted: 18 February 2020
Published online: 6 April 2020

Abstract

The reaction is responsible for destruction of the long-lived radionuclide produced during nova explosions. Since the reaction proceeds through resonances from levels in above the proton threshold at 7.581 MeV, the properties of these levels such as excitation energies, spins, and parities are crucial ingredients to determine the reaction rate. Despite recent studies of these levels, their spins are not well constrained in many cases. We have measured the transfer reaction to determine spectroscopic properties of these levels at the Holifield Radioactive Ion Beam Facility at Oak Ridge National Laboratory. The spin of the = 7.788 MeV level in is constrained to be = (3/2, 5/2) through the present work. The astrophysical reaction rate at nova temperatures is updated accordingly. Nova nucleosynthesis model calculations using the newly updated reaction rate shows that the final weighted abundance of the radionuclide is increased by 42% compared to that obtained by using the previous reaction rate of Sallaska et al. for a 1.35 ONeMg white dwarf.