6533b85dfe1ef96bd12bdbbc

RESEARCH PRODUCT

De-excitation of the strongly coupled band in Au177 and implications for core intruder configurations in the light Hg isotopes

B. SaygiE. A. LawrieWouter RyssensJuha UusitaloSanna StolzeM. VeselskýPauli PeuraPaul-henri HeenenT. GrahnM. BaloghC. ScholeyA. HerzáňA. HerzáňUlrika JakobssonPanu RuotsalainenKalle AuranenJoonas KonkiP. RahkilaMichaël BenderJ. L. WoodF. A. AliF. A. AliB. BallyM. SedlákC. McpeakeDavid O'donnellRobert PageD. T. JossMatti LeinoM. VenhartA. ThornthwaiteR. JulinAndrei AndreyevAndrei AndreyevJari PartanenJanne PakarinenJuha SorriJan SarénMikael SandzeliusJ. L. EastonPaul GreenleesRaymond J. CarrollD. KĺčV. MatoušekS. Juutinen

subject

PhysicsIsotopeProton010308 nuclear & particles physicsNuclear TheoryCoupling (probability)01 natural sciencesExcited stateNeutron number0103 physical sciencesNeutronNuclideAtomic physicsNuclear Experiment010306 general physicsExcitation

description

Excited states in the proton-unbound nuclide $^{177}$Au were populated in the $^92}$Mo($^{88}$Sr, p2n) reaction and identified using the Jurogam-II and GREAT spectrometers in conjunction with the RITU gas-filled separator at the University of Jyvaskyla Accelerator Laboratory. A strongly coupled band and its decay path to the 11/2−α-decaying isomer have been identified using recoil-decay tagging. Comparisons with cranked Hartree-Fock-Bogoliubov (HFB) calculations based on Skyrme energy functionals suggest that the band has a prolate deformation and is based upon coupling the odd 1h11/2 proton hole to the excited 02+ configuration in the $^{178}$Hg core. Although these configurations might be expected to follow the parabolic trend of core Hg(02+) states as a function of neutron number, the electromagnetic decay paths from the strongly coupled band in $^{177}$Au are markedly different from those observed in the heavier isotopes above the midshell. This indicates that a significant change in the structure of the underlying A+1Hg core occurs below the neutron midshell.

https://doi.org/10.1103/physrevc.95.061302