First results from the INDRA-FAZIA apparatus on isospin diffusion in $^{58,64}$Ni+$^{58,64}$Ni systems at Fermi energies
C. Ciampi, S. Piantelli, G. Casini, G. Pasquali, J. Quicray, L., Baldesi, S. Barlini, B. Borderie, R. Bougault, A. Camaiani, A. Chbihi, D., Dell'Aquila, M. Cicerchia, J. A. Due\~nas, Q. Fable, D. Fabris, J. D., Frankland, C. Frosin, T. G\'enard, F. Gramegna, D. Gruyer

TL;DR
This study investigates isospin diffusion in Ni+Ni collisions at Fermi energies using the INDRA-FAZIA detector, revealing that isospin equilibration is more pronounced at lower energies and with increasing collision centrality.
Contribution
First experimental results on isospin diffusion in Ni+Ni systems at Fermi energies using the combined INDRA-FAZIA apparatus, demonstrating energy-dependent isospin equilibration.
Findings
Isospin transport ratio indicates increased equilibration with centrality.
Stronger isospin equilibration observed at 32 MeV/nucleon than at 52 MeV/nucleon.
Quasiprojectile characteristics support isospin diffusion conclusions.
Abstract
An investigation of the isospin equilibration process in the reactions Ni+Ni at two bombarding energies in the Fermi regime (MeV/nucleon and MeV/nucleon) is presented. Data have been acquired during the first experimental campaign of the coupled INDRA-FAZIA apparatus in GANIL. Selecting from peripheral to semi-central collisions, both the neutron content of the quasiprojectile residue and that of the light ejectiles coming from the quasiprojectile evaporation have been used as probes of the dynamical process of isospin diffusion between projectile and target for the asymmetric systems. The isospin transport ratio technique has been employed. The relaxation of the initial isospin imbalance with increasing centrality has been clearly evidenced. The isospin equilibration appears stronger for the reactions at MeV/nucleon, as expected due to the longer…
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Taxonomy
TopicsNuclear physics research studies · Nuclear reactor physics and engineering · Advanced Chemical Physics Studies
