Nuclear structure in the weak process JUNO-Neutrino, IHEP, July 11, 2015 Yang Sun ( 孙扬 ) Center...
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Transcript of Nuclear structure in the weak process JUNO-Neutrino, IHEP, July 11, 2015 Yang Sun ( 孙扬 ) Center...
Nuclear structure in the weak process
JUNO-Neutrino, IHEP, July 11, 2015
Yang Sun (孙扬 )Center for Nuclear Astrophysics (CNA)
Shanghai Jiao Tong University (SJTU), China
Neutrino in Wikipedia
Neutrino was postulated first by Wolfgang Pauli in 1930 to explain how beta decay could conserve energy, momentum, and angular momentum (spin).
Neutrinos can interact with a nucleus, changing it to another nucleus.
In nuclear physics, beta decay (β-decay) is a type of radioactive decay in which a proton is transformed into a neutron, or vice versa, inside an atomic nucleus. This process allows the atom to move closer to the optimal ratio of protons and neutrons.
已知 118种核素 ( 包括近年来新发现的、还未命名的 )
只有不到 300个稳定的同位素 ( 对此我们有一定认识 )
对大部份非稳定同位素有所知 , 但知之不多
对其余几千个远离稳定区的同位素性质则一无所知
The family of isotopes
s process
p process
Pb (82)
Sn (50)
Fe (26)
H (1)protons
neutrons
stellar burning
Big Bang
Cosm ic Rays
Supernovae
rp process
r process
M ass know nH alf-life know nnoth ing know n
How are the isotopes synthesized?
Neutron star
rp-process =Rapid proton capture process
One of the major processesfor heavy element production
Most of the time is spent at the waiting point nuclei
rp-process in x-ray burst
27282930 3132 333435 3637383940 4142 4344
45 464748
495051 52
535455
56
5758
5960
61 62 6364 656667 68697071 727374
75 76 7778
7980 8182
G a (31)G e (32)As (33)
Se (34)Br (35)Kr (36)Rb (37)
Sr (38) Y (39)
Zr (40)Nb (41)
M o (42)Tc (43)
Ru (44)Rh (45)Pd (46)Ag (47)
Cd (48)In (49)
Sn (50)Sb (51)
Te (52) I (53)
Xe (54)
0 20 40 60 80 100 12010
-6
10-5
10-4
10-3
10-2
68
72
76
abun
danc
e
64
104
80
Mass number
slow decay (waiting point)
Waiting point nuclei
Important role of nuclear structure in nucleosynthesis
Nuclear structure controls the clock for the stellar processes the total time along the reaction path entirely determines the
speed of nucleosynthesis towards heavier nuclei and the produced isotopic abundances
We need to know: nuclear masses (ground state properties, energy gaps, single-
particle levels, ...) nuclear structure (nuclear deformation, collective excitations,
quasiparticle excitations, isomeric states, …) capture rates -decay rates
The astrophysical processes of nucleosynthesis involve those nuclei, which are unstable isotopes. We do not know much about their properties.
These nuclei are very short-lived, close to the drip line, and therefore, are very challenging experimentally.
Some of their properties can be experimentally measured, but require new concepts in facilities.
Some of them can not be measured, even not in principle.
Request of advanced facilities
Stellar enhancement of decay rate
A stellar enhancement can result from the thermal population of excited states
Examples in the s-process
m mm
iii
i jiji
kTEI
kTEIp
p
/exp12
/exp12
F. Kaeppeler, Prog. Part. Nucl. Phys. 43 (1999) 419
Double decay is a very rare transition between two nuclei with the same mass number (A) that changes the nuclear charge (Z) by two units Typically, decay from the ground state (spin and parity 0+) of an
initial even-even nucleus to the ground state (also 0+) of an final even-even nucleus
Two-neutrino decay, (2)
conserves lepton number
Neutrinoless decay, (0)
violates lepton number – thus forbidden in the Standard Model
Double beta decay
Majorana particles are identical with their own antiparticles
Detection of the neutrinoless double decay would imply evidence of physics beyond the Standard Model and the neutrino is a massive Majorana particle
If (0) decay is by the exchange of a massive Majorana neutrino, the half-life is
Phase-space integral
Nuclear matrix elements
Neutrino mass
Majorana neutrino
A tiny value changes in nuclear structure can cause big changes in astrophysical observations
Examples: Rapid proton capture process (rp-process) of nucleosynthesis in nuclear astrophysics Changes in the waiting-point nuclear mass Occurrence of new isomers in waiting point N=Z nuclei
Study of isospin-symmetry breaking and n-p pairing could impact nuclear astrophysics
Tiny changes in nuclear structure could make it `big’ in astrophysics
These masses are measured for the first time.
It confirms that CDE (binding-energy difference between mirror nuclei) method for obtaining unknown masses is reliable at least for 63Ge, 67Se.
It shows some differences for 65As and 71Kr.
Mass measurement results in Lanzhou
89%–90% of the reaction flow passes through 64Ge via proton capture indicating that: 64Ge is not a significant rp-process waiting point.
1
Abundance of x-ray burst ashes
Stellar weak interaction rates
Study of stellar weak interaction rates in astrophysics is essentially a nuclear structure problem Pioneering work of G. Fuller, W. A. Fowler, M. J. Newman
Decay rates are determined by the microscopic content of nuclear many-body wavefunctions
Nuclear shell model (diagonalization of an effective Hamiltonian in a chosen model space) is the most preferable method for GT transition calculations. M. B. Aufderheide, S. D. Bloom, D. A. Resler, G. J. Mathews,
Phys. Rev. C 47, 2961 (1993). K. Langanke and G. Martınez-Pinedo, Rev. Mod. Phys. 75,
819 (2003).
Nuclear structure models
Description of the strongly correlated many-body systems – two popular methods:
Shell-model diagonalization method Based on quantum mechanical principles Growing computer power helps extending applications A single configuration contains no physics Huge basis dimension required, severe limit in applications
Mean-field approximations Applicable to any size of systems Fruitful physics around minima of energy surfaces No configuration mixing, results depending on quality of mean-field States with broken symmetry, usually cannot study transitions and
decay rates
Beyond the mean fields
Quasiparticle Random Phase Approximation (QRPA) is the current method for heavy nuclei, particularly for forbidden transitions Build 1p-1h correlations on top of a mean field D. Rowe, Rev. Mod. Phys. 40, 153 (1968)
Not a shell model, may contain spurious components in wavefunctions
For deformed nuclei, calculated nuclear states are usually not angular momentum states, but K-states (which are mixtures of I-states)
Development of nuclear structure theories
The group at shanghai Jiao Tong University has worked actively on the development of new shell models.
It has established the unique model using the projection method and the Pfaffian algorithm for numerical computation.
How to treat heavy, deformed nuclei
Most nuclei in the nuclear chart are deformed. To describe a deformed nucleus, a spherical shell model loses advantages.
One can start from a deformed basis by breaking the rotational symmetry spontaneously.
Then apply angular-momentum-projection technique to recover the symmetry. important correlations prepared through a good mean-field intrinsic states classified with well-defined physical meanings these states transformed to the laboratory frame diagonalization performed in the (angular-momentum)
projected basis
Novel method connecting mean-field and shell models
Angular-momentum projection method based on deformed mean-field solutions Start from intrinsic bases (e.g. solutions of deformed mean-
field) and select most relevant configurations Use angular momentum projection technique to transform
them to laboratory basis (many-body technique) Diagonalize Hamiltonian in the projected basis (configuration
mixing, a shell-model concept) It is an efficient way, and probably the only way to treat
heavy, deformed nuclei with a shell model concept
The Projected Shell Model (PSM):• K. Hara, Y. Sun, Int. J. Mod. Phys. E 4 (1995) 637
Multi-quasiparticle computation using the Pfaffian algorithm
Calculation of projected matrix elements usually uses the generalized Wick theorem
A matrix element having n (n’) qp creation or annihilation operators respectively on the left- (right-) sides of the rotation operator contains (n + n − 1)!! terms in the expression – a problem of combinatorial complexity
Use of the Pfaffian algorithm: L.M. Robledo, Phys. Rev. C 79 (2009) 021302(R). G. Bertsch, L.M. Robledo, Phys. Rev. Lett. 108 (2012) 042505. T. Mizusaki, M. Oi, Phys. Lett. B 715 (2012) 219. M. Oi, T. Mizusaki, Phys. Lett. B 707 (2012) 305. T. Mizusaki, M. Oi, F.-Q. Chen, Y. Sun, Phys. Lett. B 725 (2013) 175 Q.-L. Hu, Z.-C. Gao, Y. S. Chen, Phys. Lett. B 734 (2014) 162.
L.-J. Wang et al. Phys. Rev. C90 (2014) 011303(R)
A third band-crossing is described.
Extension of configuration space to 6-qps.
Associated institution of JINA-CEE Promote nuclear astrophysics development in China Promote international collaborations and academic
exchanges in this field Carry out conversations from different fields in China
Nuclear experimental facilities in IMP (Lanzhou), CIAE (Beijing) JinPing underground lab (Sichuan) JiangMen neutrino lab (Guangdong) Shanghai synchrotron light (upgrade to provide gamma rays) Strong laser facilities (ShenGuang) Large telescope LAMOST (Beijing) Supercomputer Tian-He (Tianjin)
Nuclear astrophysics center at Shanghai Jiao Tong University
Summary
The discovery of neutrinos was made in nuclear physics through beta decay.
In nuclear physics, weak processes occur in parent nuclei, and therefore, the knowledge of nuclear many-body systems is involved.
Some quantities can be measured experimentally, but many others have to rely on theoretical calculations.
It defines a close relation between neutrino physics and nuclear physics.