Superallowed Gamow-Teller decay of the doubly magic nucleus $^{100}$Sn
C.B. Hinke
,
M. Böhmer
,
P. Boutachkov
,
T. Faestermann
,
H. Geissel
,
J. Gerl
,
R. Gernhauser
,
M. Gorska
,
A. Gottardo
,
H. Grawe
,
J. L. Grebosz
,
R. Krûcken
,
N. Kurz
,
Z. Liu
,
L. Maier
,
F. Nowacki
(1)
,
S. Piétri
,
Zs. Podolyak
,
K. Sieja
(1)
,
K. Steiger
,
K. Straub
,
H. Weick
,
P. J.Woods
,
N. Al-Dahan
,
N. Alkhomashi
,
A. Ataç
,
A. Blazhev
,
N. F. Braun
,
I.T. Celikovic
,
T. Davinson
,
I. Dillmann
,
C. Domingo-Pardo
,
P. C. Doornenbal
,
G. de France
(2)
,
G. F. Farrelly
,
F. Farinon
,
N. Goel
,
T.C. Habermann
,
R. Hoischen
,
R. Janik
,
M. Karny
,
A. Kaskas
,
I.M. Kojouharov
,
Th. Kroll
,
Y. Litvinov
,
S. Myalski
,
F. Nebel
,
S. Nishimura
,
C. Nociforo
,
J. Nyberg
,
A. R. Parikh
,
A. Prochazka
,
P. H. Regan
,
C. Rigollet
,
H. Schaffner
,
C. Scheidenberger
,
S. Schwertel
,
P.-A. Soderstrom
,
S.J. Steer
,
A. Stolz
,
P. Strmen
C.B. Hinke
- Function : Author
M. Böhmer
- Function : Author
P. Boutachkov
- Function : Author
T. Faestermann
- Function : Author
H. Geissel
- Function : Author
J. Gerl
- Function : Author
R. Gernhauser
- Function : Author
M. Gorska
- Function : Author
A. Gottardo
- Function : Author
H. Grawe
- Function : Author
J. L. Grebosz
- Function : Author
R. Krûcken
- Function : Author
N. Kurz
- Function : Author
Z. Liu
- Function : Author
L. Maier
- Function : Author
F. Nowacki
- Function : Author
- PersonId : 748924
- IdHAL : frederic-nowacki
- ORCID : 0000-0002-7854-8717
S. Piétri
- Function : Author
Zs. Podolyak
- Function : Author
K. Sieja
- Function : Author
- PersonId : 738608
- IdHAL : kamila-sieja
- ORCID : 0000-0001-7736-656X
K. Steiger
- Function : Author
K. Straub
- Function : Author
H. Weick
- Function : Author
P. J.Woods
- Function : Author
N. Al-Dahan
- Function : Author
N. Alkhomashi
- Function : Author
A. Ataç
- Function : Author
A. Blazhev
- Function : Author
N. F. Braun
- Function : Author
I.T. Celikovic
- Function : Author
T. Davinson
- Function : Author
I. Dillmann
- Function : Author
C. Domingo-Pardo
- Function : Author
P. C. Doornenbal
- Function : Author
G. F. Farrelly
- Function : Author
F. Farinon
- Function : Author
N. Goel
- Function : Author
T.C. Habermann
- Function : Author
R. Hoischen
- Function : Author
R. Janik
- Function : Author
M. Karny
- Function : Author
A. Kaskas
- Function : Author
I.M. Kojouharov
- Function : Author
Th. Kroll
- Function : Author
Y. Litvinov
- Function : Author
S. Myalski
- Function : Author
F. Nebel
- Function : Author
S. Nishimura
- Function : Author
C. Nociforo
- Function : Author
J. Nyberg
- Function : Author
A. R. Parikh
- Function : Author
A. Prochazka
- Function : Author
P. H. Regan
- Function : Author
C. Rigollet
- Function : Author
H. Schaffner
- Function : Author
C. Scheidenberger
- Function : Author
S. Schwertel
- Function : Author
P.-A. Soderstrom
- Function : Author
S.J. Steer
- Function : Author
A. Stolz
- Function : Author
P. Strmen
- Function : Author
Abstract
The shell structure of atomic nuclei is associated with 'magic numbers' and originates in the nearly independent motion of neutrons and protons in a mean potential generated by all nucleons. During b1-decay, a proton transforms into a neutron in a previously not fully occupied orbital, emitting a positron-neutrino pair with either parallel or antiparallel spins, in a Gamow-Teller or Fermi transition, respectively. The transition probability, or strength, of a Gamow-Teller transition depends sensitively on the underlying shell structure and is usually distributed among many states in the neighbouring nucleus. Here we report measurements of the half-life and decay energy for the decay of 100Sn, the heaviest doubly magic nucleus with equal numbers of protons and neutrons. In the b-decay of 100Sn, a large fraction of the strength is observable because of the large decay energy. We determine the largest Gamow-Teller strength so far measured in allowed nuclear b-decay, establishing the 'superallowed' nature of this Gamow-Teller transition. The large strength and the low-energy states in the daughter nucleus, 100In, are well reproduced by modern, large-scale shell model calculations.