Nuclear beta decay

Behrens, H.; Bühring, Wolfgang

doi:10.1016/0375-9474(71)90489-1

Cited by 144 publications

(131 citation statements)

References 12 publications

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“…To evaluate the contribution of the square bracket we can use the expressions for U(r) and l(r) listed in Table 3 of [16]. For such a calculation we have to consider separately two regions one inside and another outside the nuclear radius.…”

Section: The Dependence Of ~T-on the Ips Interactionmentioning

confidence: 99%

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The decay of theT=1 isospin triplet inA=12 systems: II. The induced interactions in the anisotropy of beta-rays

Szybisz

1978

Z Physik A

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Nuclear Structure: calculation of the asymmetry a T of fl rays emitted from polarized t2B and 12 N nuclei. Comparison with experimental values.Formulae for the asymmetry parameters a v of fl rays emitted from polarized nuctei is derived using the formalism developed by Behrens-Biihring. The induced interactions are studied in detail. It is demonstrated that the expressions for a_ v are independent of the induced pseudoscalar interaction. It was found that the corrections to the lowest order approximation are small. Experimental data of the Louvain and Osaka laboratories are analyzed. We should point out that the data of the asymmetry of the fl-decay of 12B obtained in these two laboratories are quite different. Although the data reported by the Osaka Group require the existence of the induced pseudotensor (IPT) interaction as it, has also been stated by other authors, if we combine data of 12N from Osaka and of lZB from Lauvain such experimental results can be understood without including the IPT interaction. Thus, we found some evidence that the IPT interaction could be not necessary to explain the asymmetries in the decay of members of the A = 12 system.

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Section: The Dependence Of ~T-on the Ips Interactionmentioning

confidence: 99%

“…For this purpose we can write the numerator using for D o and D 1 the complete expressions (16) and (17), respectively,…”

Section: Iv2 the Higher Order Correctionsmentioning

confidence: 99%

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The decay of theT=1 isospin triplet inA=12 systems: II. The induced interactions in the anisotropy of beta-rays

Szybisz

1978

Z Physik A

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“…However, in many applications the momentum transfers involved are small compared with the typical nuclear momentum Q ≈ R −1 , with R the nuclear radius. In that case, the above formulas can be expanded in powers of (qR) (long-wavelength limit) and one obtains the standard approximations to allowed (Gamow-Teller and Fermi) and forbidden transitions (Bambynek et al, 1977;Bühring, 1971, 1982). In these limits the effect of the electromagnetic interaction on the initial or final charged lepton, that has been neglected in the above expressions, can be included (Schopper, 1966).…”

Section: Introductionmentioning

confidence: 99%

Nuclear weak-interaction processes in stars

2003

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Recent experimental data and progress in nuclear structure modeling have lead to improved descriptions of astrophysically important weak-interaction processes. The review discusses these advances and their applications to hydrostatic solar and stellar burning, to the slow and rapid neutron-capture processes, to neutrino nucleosynthesis, and to explosive hydrogen burning. Special emphasis is given to the weak-interaction processes associated with core-collapse supernovae. Despite some significant progress, important improvements are still warranted. Such improvements are expected to come from future radioactive ion-beam facilities.Comment: 45 pages, 33 figures, REVTeX 4, submitted to Rev. Mod. Phys., modified following referee's comment

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“…The release of nuclear energy happens when nucleons rearrange themselves to form more stable nuclei. In such nuclear reaction processes, a large amount of energy is released in the form of emitted kinetic energy of particles or fragments and electromagnetic radiation.There are three ways to release nuclear energy, known as radioactive decay [1][2][3][4], fusion [5][6][7][8][9][10] and fission [11][12][13][14][15]. The radioactive decay is the spontaneous process which occurs in radioactive materials by which the nuclei of unstable parent nuclei, gradually break up and are transformed into more stable isotopes or into nuclei of a different type.…”

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Nuclear energy release from fragmentation

Souza

Tsang

et al. 2016

Nuclear Physics A

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Abstract. Nuclear energy released by splitting Uranium and Thorium isotopes into two, three, four, up to eight fragments with nearly equal size are studied. We found that the energy released from equally splitting the 235,238 U and 230,232 Th nuclei into to three fragments is largest. The statistical multifragmentation model is employed to calculate the probability of different breakup channels for the excited nuclei. Weighing the the probability distributions of fragments multiplicity at different excitation energies for the 238 U nucleus, we found that an excitation energy between 1.2 and 2 MeV/u is optimal for the 235 U, 238 U, 230 Th and 232 Th nuclei to release nuclear energy of about 0.7-0.75 MeV/u. ‡ Email: imqmd@qq.com § Corresponding author: fszhang@bnu.edu.cn Nuclear energy release from fragmentation 2 Nuclear energy is one of the most efficient sources of energy based on the Einstein's mass-energy equivalence formula (∆E = ∆mc 2 ). It originates in the strong force holding the protons and neutrons together. The release of nuclear energy happens when nucleons rearrange themselves to form more stable nuclei. In such nuclear reaction processes, a large amount of energy is released in the form of emitted kinetic energy of particles or fragments and electromagnetic radiation.There are three ways to release nuclear energy, known as radioactive decay [1][2][3][4], fusion [5][6][7][8][9][10] and fission [11][12][13][14][15]. The radioactive decay is the spontaneous process which occurs in radioactive materials by which the nuclei of unstable parent nuclei, gradually break up and are transformed into more stable isotopes or into nuclei of a different type. The daughter nuclei, consequently lose energy by emitting radiation in the form of particles (include α, β, photons, neutrons particle etc.) and/or electromagnetic waves. The continuous fusion reaction happens in the core of stars including our sun. However in order to harness it to produce power, the fusion process must be controlled. Nuclear energy from fusion is still far from commercially viable even though controllable fusion reaction has been studied for many years through the means of magnetic confinement [16][17][18] and inertial confinement [19][20][21][22]. The fission technology has been widely used to generate power by neutron-induced chain reactions. This fission process occurs when a heavy nucleus such as 235 U and 239 Pu absorbs a thermal neutron and the excited compound nucleus is excited to be near its fission barrier. At low excitation energy, quantum effects in the fission process are very significant to the dynamical evolution of the system. Nuclear structure effects, such as the shell corrections, directly influence the fission barrier height and the fission path. Most fission modes induced by thermal neutron are binary fissions in which one daughter nucleus has a mass of about 90 to 100 u and the remaining nucleus 130 to 140 u. Occasionally ternary fission and quaternary fission occur with relatively probability of 1/300 and 1/3000 per ...

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Nuclear beta decay

Cited by 144 publications

References 12 publications

The decay of theT=1 isospin triplet inA=12 systems: II. The induced interactions in the anisotropy of beta-rays

The decay of theT=1 isospin triplet inA=12 systems: II. The induced interactions in the anisotropy of beta-rays

Nuclear weak-interaction processes in stars

Nuclear energy release from fragmentation

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