Neutron-spectroscopic factors for low-lying 16N levels
D. W. Bardayan, ORNL Physics Division
P. D. O'Malley, Rutgers University–New Brunswick
J. C. Blackmon, Louisiana State University
K. Y. Chae, The University of Tennessee, Knoxville
K. A. Chipps, Colorado School of Mines
J. A. Cizewski, Rutgers University–New Brunswick
R. Hatarik, Rutgers University–New Brunswick
K. L. Jones, The University of Tennessee, Knoxville
R. L. Kozub, Tennessee Technological University
C. Matei, Oak Ridge Assoct. Universities
B. H. Moazen, The University of Tennessee, Knoxville
C. D. Nesaraja, ORNL Physics Division
S. D. Pain, ORNL Physics Division
S. Paulauskas, The University of Tennessee, Knoxville
W. A. Peters, Rutgers University–New Brunswick
S. T. Pittman, Rutgers University–New Brunswick
K. T. Schmitt, The University of Tennessee, Knoxville
J. F. Shriner, Tennessee Technological University
M. S. Smith, ORNL Physics Division
Abstract
The magnitude of the 15N(n,γ)16N reaction rate in asymptotic giant branch stars depends directly on the neutron spectroscopic factors of low-lying 16N levels. A new study of the 15N(d,p)16N reaction is reported populating the ground and first three excited states in 16N. The preliminary spectroscopic factors are near unity as expected from shell model calculations, resolving a longstanding discrepancy with previous experiments. The data and analysis are presented. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlikeLicence.
