Isoscalar Transition Rates in Nuclei from the (α, α′) Reaction

Bernstein, A. M.

doi:10.1007/978-1-4757-9018-4_5

Cited by 103 publications

(20 citation statements)

References 114 publications

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“…The j > ↔ j < transition and the transitions between the same orbits (i.e., j > ↔ j > and j < ↔ j < ) are separated, in first order, by 3 to 6 MeV, the separation in energy of the spin-orbit partners. (5) In contrast to the Fermi transitions, where only the T z is changed by the τ operator and hence only a single state [the so-called Isobaric Analog State (IAS)] is populated in the final nucleus, GT transitions involve both the σ and the τ operators and a variety of different states can be populated. As a result one can extract more information about nuclear structure in the final nucleus.…”

Section: Properties Of Gamow-teller Transitionsmentioning

confidence: 99%

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Weak interaction in nuclear astrophysics

Fujita¹

2013

Proceedings of VI European Summer School on Experimental Nuclear Astrophysics — PoS(ENAS 6)

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Study of nuclear weak processes, especially the Gamow-Teller (GT) transitions, starting from stable as well as unstable nuclei, is one of the key issues in nuclear physics and nuclear astrophysics. In the collapsing core of pre-supernova stars, where the temperature of a few ×10 9 K is expected, electron capture and neutrino induced reactions play important roles. In these reactions, GT transition is one of the main actors. However, due to the weakness of the weak interaction causing these reactions, experimental study of these reactions that can happen under such extreme stellar conditions are difficult. Direct information on GT transitions and the GT transition strength B(GT) by using the weak interaction itself has been available only from β -decay measurements. However, B(GT) values are usually derived only for low-lying states. Note that the study of the feedings to higher excited states is difficult in a β -decay study, because the phase-space factor ( f -factor) decreases with the excitation energy. The GT transitions are caused by the σ τ-type operator. It is known that the nuclear excitation by means of the σ τ-type nuclear strong interaction becomes dominant in charge-exchange (CE) reactions performed at small scattering angles and intermediate incident energies. Therefore, we study the GT transitions using hadronic ( 3 He,t), CE reactions. By realizing dispersion matching conditions, high energy-resolution has been realized and detailed GT strength distributions can be studied up to high excitation energies. Under the assumption that isospin is a good quantum number, symmetry is expected for the structure of mirror nuclei and the GT transitions starting from them. The results from ( 3 He,t) reactions on stable p f -shell nuclei are compared and also combined with the complementary β -decay studies for the mirror proton-rich nuclei in the region far-from-stability. Since the pass of the rp-process nucleosynthesis goes thorough these proton-rich nuclei, the information on GT transitions from them are essential for the better understanding of the process.

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Section: Properties Of Gamow-teller Transitionsmentioning

confidence: 99%

“…Thus, each mode of excitation should be distinguished by the type of operator exciting the mode. For the simplest cases of IS electric transitions, it is usual to assume a type of operator [5,6] with the form…”

Section: Gamow-teller Transitionsmentioning

confidence: 99%

Weak interaction in nuclear astrophysics

Fujita¹

2013

Proceedings of VI European Summer School on Experimental Nuclear Astrophysics — PoS(ENAS 6)

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“…For oddmass nuclei the weak coupling model [16] was adopted. The values of 0)2, f12 and 0)3 are taken from [16][17][18] whereas for 2=3 the parametrization f12 = (22 + 1)0)~/(2Ca) with C 3 = 500 MeV was used (see Table 1). All delta functions entering (8 b) are replaced by Gaussians of width 0.7 MeV simulating both the limited (exit channel) energy resolution in experiments and the spreading of spectroscopic strength.…”

Section: (3)mentioning

confidence: 99%

Description of (n, p) and (n, 2n-activation cross sections for medium-mass nuclei within statistical multistep theory

Kalka

Torjman

Lien

et al. 1990

Z. Physik A - Atomic Nuclei

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“…Use of the A L= 1 form factor suggested by Satchler [12] gave predictions very near in shape and magnitude to those for a first derivative only. A microscopic [13] alpha-nucleon interaction of Gaussian form [14] and the use of oscillator radial wave functions permit the analytic computation of transition form factors for promoting alp shell nucleon into the ld or 2s orbitals. These radial form factors are presented in [15].…”

Section: The Experiments and Analysismentioning

confidence: 99%

Alpha particle scattering to negative parity states of14N

Peterson

Hamill

1982

Z Physik A

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Inelastic SHe scattering on melamine targets is studied for negative parity excitations of 14N. Eleven AL=3 excitations are presented, for states up to 15.41 MeV; three AL= 1 transitions are also studied. A microscopic DWBA calculation accounts for several of the octupole excitations, requiring an isoscalar effective strength about twice that expected for free alpha-nucleon scattering. Great purity of the structure of the three lowest 2-states is noted, with the 5.11 MeV and 9.13 MeV levels excited by AL=3, but with the 7.97 MeV state excited purely by AL = 1.Nuclear Reactions: 14N(4He, SHe'), E~=34.85 MeV; measured cr(E~, 0), deduced/3 and microscopic interaction strengths through DWBA.

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Isoscalar Transition Rates in Nuclei from the (α, α′) Reaction

Cited by 103 publications

References 114 publications

Weak interaction in nuclear astrophysics

Weak interaction in nuclear astrophysics

Description of (n, p) and (n, 2n-activation cross sections for medium-mass nuclei within statistical multistep theory

Alpha particle scattering to negative parity states of14N

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