Physics Letters B 797 (2019) 134820
Contents lists available at ScienceDirect
Physics Letters B
www.elsevier.com/locate/physletb
First experimental constraint of the spectroscopic amplitudes for the
α-cluster in the
11
Bground state
Y.P. Shen ( )
a
, B. Guo ( )
a,∗
, T.L. Ma ( )
a
, D.Y. Pang ( )
b,c
, D.D. Ni
(
)
d
, Z.Z. Ren ( )
e
, Y.J. Li ( )
a
, Z.D. An ( )
f
, J. Su ( )
a
, J.C. Liu
(
)
a
, Q.W. Fan ( )
a
, Z.Y. Han ( )
a
, X.Y. Li ( )
a
, Z.H. Li ( )
a
, G. Lian
(
)
a
, Y. Su ( )
a
, Y.B. Wang ( )
a
, S.Q. Yan ( )
a
, S. Zeng ( )
a
, W.P. Liu
(
)
a
a
China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, China
b
School of Physics and Nuclear Energy Engineering, Beihang University, Beijing 100191, China
c
Beijing Key Laboratory of Adv anced Nuclear Materials and Physics, Beihang University, Beijing 100191, China
d
Space Science Institute, Macao University of Science and Technology, Macao, China
e
School of Physics Science and Engineering, Tongji University, Shanghai 200092, China
f
School of Physics and Astronomy, Sun Yat-Sen University, Zhuhai 519082, China
a r t i c l e i n f o a b s t r a c t
Article history:
Received
30 November 2018
Received
in revised form 3 July 2019
Accepted
27 July 2019
Available
online 31 July 2019
Editor:
D.F. Geesaman
We present the first experimental determination on the spectroscopic amplitudes (SAs) for the α-cluster
in the
11
Bground state via the
7
Li(
6
Li, d)
11
Breaction using a high-precision magnetic spectrograph. This
is believed to have a strong effect on the studies of α-induced reactions which are crucial in nuclear
astrophysics. It is found that the previous SAs of
11
Bfrom shell model calculations cause overestimations
of up to 23% for the
12
C(α, γ )
16
O S
E2
(300) factor and up to 34% for the
13
C(α, n)
16
O S(190) factor
with respect to the results from the present experimentally determined SAs. Due to the importance of
these two reactions, for example the uncertainty in the
12
C(α, γ )
16
Ocross section at E
c.m.
= 300 keV is
required to be better than 10% by stellar modeling, the new S-factors could result in a potential influence
on the astrophysical network calculations.
© 2019 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license
(http://creativecommons.org/licenses/by/4.0/). Funded by SCOAP
3
.
1. Introduction
A nuclear cluster can be defined as a spatially located subsys-
tem
which consists of the strongly correlated nucleons. The clus-
tering
in nuclei is one of the most fundamental aspects in nuclear
structure and has been investigated since the early days in the his-
tory
of nuclear physics [1]. The research of the cluster structure
in light nuclei is also an interesting topic [2]. It could generate
a crucial impact on the synthesis of elements in stars via cluster
states like the triple-α cluster state (so-called Hoyle state) at 7.65
MeV in
12
C[3,4]. A cluster is characterized by its intrinsic bind-
ing
stronger than the external binding. Therefore, it is possible to
consider the cluster as a single unit, and to describe its behavior
without reference to its internal structure. The most likely cluster
is, due to its spin and isospin symmetry and hence its high bind-
*
Corresponding author.
E-mail
address: guobing@ciae.ac.cn (B. Guo).
ing energy, the α-particle which can propagate within a nucleus
relatively unperturbed for a significant time [5]. Such a cluster can
be knocked out of the nucleus by an energetic projectile, or it can
be also picked up in a cluster-transfer reaction. These cluster reac-
tions
provide important information on the single-particle and on
the multi-particle character of nuclear states, and thus have been
widely used as powerful nuclear spectroscopic tools [6].
The
α-transfer reactions, being most likely to take place by
cluster transfer, not only can be utilized to investigate nuclear
structure (e.g., α-decay widths [7]) and nuclear reaction mecha-
nisms
[6], but also are of particular interest for the study of as-
trophysical
α-particle induced reactions [8] which are one kind of
the most important reactions in nuclear astrophysics, since helium
is the second most abundant element in the observable universe
after hydrogen. Because the measurements of the α-particle in-
duced
reactions at the low-energy range are greatly hindered by
the Coulomb barrier, indirect techniques (e.g., α-transfer reactions)
are extremely valuable. In particular, these techniques can be used
to deduce the level parameters (i.e., energies, spectroscopic factors
https://doi.org/10.1016/j.physletb.2019.134820
0370-2693/
© 2019 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/). Funded by
SCOAP
3
.
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