Determination of the Gamow-Teller Quenching Factor via the90Zr(n, p) Reaction at 293 MeV

2003 ◽  
Author(s):  
K. Yako
Keyword(s):  
Quenching Factor ◽  
Gamow Teller

DETERMINATION OF THE GAMOW-TELLER QUENCHING FACTOR VIA THE 90Zr(n, p) REACTION AT 293 MEV

2003 ◽  
Author(s):  
K. YAKO ◽  
H. SAKAI ◽  
M. HATANO ◽  
H. KATO ◽  
Y. MAEDA ◽  
...  
Keyword(s):  
Quenching Factor ◽  
Gamow Teller

scholarly journals Determination of the Gamow–Teller quenching factor from charge exchange reactions on 90Zr

2005 ◽  
Vol 615 (3-4) ◽  
pp. 193-199 ◽  
Author(s):  
K. Yako ◽  
H. Sakai ◽  
M.B. Greenfield ◽  
K. Hatanaka ◽  
M. Hatano ◽  
...  
Keyword(s):  
Charge Exchange ◽  
Exchange Reactions ◽  
Quenching Factor ◽  
Gamow Teller

scholarly journals On the quenching of Gamow–Teller strength

1987 ◽  
Vol 65 (6) ◽  
pp. 574-577 ◽  
Author(s):  
J. Rapaport
Keyword(s):  
Cross Sections ◽  
Wave Functions ◽  
Light Nuclei ◽  
Final States ◽  
Excitation Energies ◽  
Intermediate Energies ◽  
Quenching Factor ◽  
Configuration Mixing ◽  
Gamow Teller ◽  
Model Strength

The (p, n) reaction at intermediate energies has been used to measure differential cross sections in light nuclei to final states characterized with a ΔJπ = 1+ transfer (Gamow–Teller (GT) states). Experimental ft values for allowed beta-decay transitions in these nuclei are used to normalize the strength of the GT transitions in units of B(GT). This experimental GT strength is compared with predicted shell–model strength. For p-shell nuclei, the calculated excitation energies of the GT strength using Cohen and Kurath wave functions are in general agreement with the empirical GT distribution. Up to an excitation energy of about 20 MeV, the total experimental and calculated GT strengths are used to obtain the quenching factor, QF = Σ B(GT)exp/Σ B(GT)theor. It is found that QF decreases as the shell gets filled-up. The lowest value seems to occur for single-hole nuclei. This decrease may be explained by configuration mixing not specifically included in the calculations.

Determination of the Gamow–Teller strength function for the neutron-deficient isotopes 104–107In

2001 ◽  
Vol 690 (4) ◽  
pp. 367-381 ◽  
Author(s):  
M. Karny ◽  
L. Batist ◽  
B.A. Brown ◽  
D. Cano-Ott ◽  
R. Collatz ◽  
...  
Keyword(s):  
Strength Function ◽  
Gamow Teller

scholarly journals Determination of GT-transition Strengths in \(A=34\) Isobars Using Charge Exchange \((^3\text{He},t)\) Reaction

2012 ◽  
Vol 22 (1) ◽  
pp. 91-96
Author(s):  
Nguyen Tuan Khai ◽  
Bui Duy Linh ◽  
Tran Duc Thiep ◽  
Y. Fujita ◽  
T Adachi ◽  
...  
Keyword(s):  
Excitation Energy ◽  
Excited States ◽  
Ground State ◽  
Incident Energy ◽  
High Energy ◽  
High Energy Resolution ◽  
Good Quantum Number ◽  
Gamow Teller ◽  
Good Agreement

Under the assumption that isospin \(T\) is a good quantum number, mirror transitions \(T_{z }= +1 \to  0\) and \(T_{z }= -1  \to  0\) were studied in \(A = 34\) isobars, where \(T_{z}\) is \(z\) component of iospin \(T\) and is defined by \(T_{z} = (N-Z)/2\). With a high energy resolution of 35 keV in \(^{34}\)S\((^{3}He,t)^{34}\)Cl reaction measurement at \(0^{\circ}\) scattering angle and at an incident energy of 140 MeV/nucleon, strengths of Fermi and Gamow-Teller (GT) transitions from the \(J^{\pi } = 0^{ + }\), \(T_{z }= +1\) ground state of \(^{34}\)S to the \(J^{\pi } = 1^{+ }\), \(T_{z }= 0\) excited states in \(^{34}\)Cl were determined up to excitation energy \((E_{x})\) of \(7.08\) MeV. The corresponding isospin-symmetric transitions connecting \(T_{z }= -1\) and \(T_{z }= 0\) states can be studied in the \(^{34}\)Ar \(\beta ^{ + }\) decay. The strengths of the \((GT)_{\pm }\) transitions were compared up to the excitation energy of 3.1 MeV. A good agreement was observed for two strong transitions to \(2.580\) MeV and \(3.129\) MeV states, while a disagreement about \(45\text{%}\) was observed for a weaker transition to \(0.666\) MeV low-lying state.

scholarly journals Galactic cosmic ray hydrogen spectra and radial gradients in the inner heliosphere measured by the HELIOS Experiment 6

2019 ◽  
Vol 625 ◽  
pp. A153 ◽  
Author(s):  
J. Marquardt ◽  
B. Heber
Keyword(s):  
Operation Time ◽  
Solar Energetic Particle ◽  
Cosmic Ray ◽  
Solar Observation ◽  
Temperature Dependent ◽  
Outer Heliosphere ◽  
Quenching Factor ◽  
Galactic Cosmic Ray ◽  
Inner Heliosphere

Context. The HELIOS solar observation probes provide unique data regarding their orbit and operation time. One of the onboard instruments, the Experiment 6 (E6), is capable of measuring ions from 4 to several hundred MeV nucleon−1. Aims. In this paper we aim to demonstrate the relevance of the E6 data for the calculation of galactic cosmic ray (GCR), anomalous cosmic ray (ACR), and solar energetic particle (SEP) fluxes for different distances from the sun and time periods. Methods. Several corrections have been applied to the raw data: determination of the Quenching factor of the scintillator, correction of the temperature dependent electronics, degradation of the scintillator as well as the effects on the edge of semi-conductor detectors. Results. Fluxes measured by the E6 are in accordance with the force field solution for the GCR and match models of the anomalous cosmic ray propagation. GCR radial gradients in the inner heliosphere show a different behaviour than in the outer heliosphere.

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