2014/08/20 by Muneeb-Ur Rahman, Jameel-Un Nabi · 1 citation
Physics and Astronomy · #astro-ph.SR #nucl-th
paper · pdf · doi:10.1007/s10509-013-1580-5
published as Astrophysics and Space Science 348, 427-435 (2013) · 13 pages, 4 figures and 1 table. arXiv admin note: text overlap with arXiv:1203.4669
arxiv created 2014/08/20 · arxiv updated 2015/06/22
The Gamow-Teller strength distribution function, B(GT), for the odd Z parent 51V, N-Z =5, up to 30 MeV of excitation energy in the daughter 51Ti is calculated in the domain of proton-neutron Quasiparticle Random Phase Approximation (pn-QRPA) theory. The pn-QRPA results are compared against other theoretical calculations, (n, p) and high resolution (d, 2He) reaction experiments. For the case of (d, 2He) reaction the calibration was performed for 0≤ Ej ≤ 5.0 MeV, where the authors stressed that within this excitation energy range the ΔL = 0 transition strength can be extracted with high accuracy for 51V. Within this energy range the current pn-QRPA total B(GT) strength 0.75 is in good agreement with the (d, 2He) experiment's total strength of 0.9 ± 0.1. The pn-QRPA calculated Gamow-Teller centroid at 4.20 MeV in daughter 51Ti is also in good agreement with high resolution (d, 2He) experiment which placed the Gamow-Teller centroid at 4.1 ± 0.4 MeV in daughter 51Ti. The low energy detailed Gamow-Teller structure and Gamow-Teller centroid play a sumptuous role in associated weak decay rates and consequently affect the stellar dynamics. The stellar weak rates are sensitive to the location and structure of these low-lying states in daughter 51Ti. The calculated electron capture rates on 51V in stellar matter are also in good agreement with the large scale shell model rates.