Pathway for the Production of Neutron-Rich Isotopes around the N = 126 Shell Closure
Y.X. Watanabe
(1)
,
Y.H. Kim
(2)
,
S.C. Jeong
(1)
,
Y. Hirayama
(1)
,
N. Imai
(1)
,
H. Ishiyama
(1)
,
H.S. Jung
(1)
,
H. Miyatake
(1)
,
S. Choi
(2)
,
J.S. Song
(2)
,
E. Clément
(3)
,
G. de France
(3)
,
A. Navin
(3)
,
M. Rejmund
(3)
,
C. Schmitt
(3)
,
G. Pollarolo
(4)
,
L. Corradi
(5)
,
E. Fioretto
(5)
,
D. Montanari
(6)
,
M. Niikura
(7)
,
D. Suzuki
(7)
,
H. Nishibata
(8)
,
J. Takatsu
(8)
1
High energy accelerator research organization -
KEK
2 SNU - Seoul National University [Seoul]
3 GANIL - Grand Accélérateur National d'Ions Lourds
4 INFN, Sezione di Torino - Istituto Nazionale di Fisica Nucleare, Sezione di Torino
5 LNL - Laboratori Nazionali di Legnaro
6 INFN, Sezione di Padova - Istituto Nazionale di Fisica Nucleare, Sezione di Padova
7 IPNO - Institut de Physique Nucléaire d'Orsay
8 Osaka University [Osaka]
2 SNU - Seoul National University [Seoul]
3 GANIL - Grand Accélérateur National d'Ions Lourds
4 INFN, Sezione di Torino - Istituto Nazionale di Fisica Nucleare, Sezione di Torino
5 LNL - Laboratori Nazionali di Legnaro
6 INFN, Sezione di Padova - Istituto Nazionale di Fisica Nucleare, Sezione di Padova
7 IPNO - Institut de Physique Nucléaire d'Orsay
8 Osaka University [Osaka]
Résumé
Absolute cross sections for isotopically identified products formed in multinucleon transfer in the
136Xe + 198Pt system at ∼ 8 MeV=nucleon are reported. The isotopic distributions obtained using a large
acceptance spectrometer demonstrated the production of the “hard-to-reach” neutron-rich isotopes for
Z < 78 around the N = 126 shell closure far from stability. The main contribution to the formation of these
exotic nuclei is shown to arise in collisions with a small kinetic energy dissipation. The present
experimental finding corroborates for the first time recent predictions that multinucleon transfer reactions
would be the optimum method to populate and characterize neutron-rich isotopes around N = 126 which
are crucial for understanding both astrophysically relevant processes and the evolution of “magic” numbers
far from stability.