Phys.Rev. C 100, 045805 (2019)

R.Titus, E.M.Ney, R.G.T.Zegers, D.Bazin, J.Belarge, P.C.Bender, B.A.Brown, C.M.Campbell, B.Elman, J.Engel, A.Gade, B.Gao, E.Kwan, S.Lipschutz, B.Longfellow, E.Lunderberg, T.Mijatovic, S.Noji, J.Pereira, J.Schmitt, C.Sullivan, D.Weisshaar, J.C.Zamora

Constraints for stellar electron-capture rates on ⁸⁶Kr via the ⁸⁶Kr(t, ³He+γ)⁸⁶Br reaction and the implications for core-collapse supernovae

NUCLEAR REACTIONS ⁸⁶Kr, ¹²C, ¹⁴N(t, ³He), E=115 MeV/nucleon, [tritons from ⁹Be(¹⁶O, X), E=150 MeV/nucleon primary reaction, and separated using A1900 fragment separator]; measured ³He spectra, Eγ, Iγ, γγ- and (³He)γ-coin, differential σ(θ) using S800 spectrograph for particles and GRETINA array for γ detection at the NSCL-MSU facility. Data from ¹²C ¹⁴N present as contaminants used for energy calibration. ⁸⁶Br; deduced levels, L-transfers, Gamow-Teller strength distributions. ⁸⁶Kr; calculated electron capture rates at T=10 GK using the deduced Gamow-Teller strength distributions. Comparison with shell-model and quasiparticle random-phase approximation (QRPA) calculations. Z=26-41, N=75-93; calculated electron capture rates for 78 nuclides near N=50 and Z=28 (see 2018Ti02) using quasiparticle random-phase approximation (QRPA), with Jπ assignments made for ground states of some nuclides using Gallagher-Moszkowski (GM) rule. Relevance to astrophysical simulations of core-collapse supernovae.

doi: 10.1103/PhysRevC.100.045805