Gamow-Teller strength functions of superfluid odd-A nuclei and neutrino capture reactions

Borzov, I. N.; Fayans, S.A.; Trykov, E.L.

doi:10.1016/0375-9474(94)00769-j

Cited by 54 publications

(29 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Neglecting the effective pp interaction, as was done, e.g., in [5], would destroy the symmetry of the QRPA equations and cause unrealistic odd-even staggering of total β-decay half-lives. Notice, that for odd-A nuclei, the FFS equations account properly for the odd-particle transitions [19].…”

Section: β-Strength Functionmentioning

confidence: 99%

See 1 more Smart Citation

β-delayed neutron emission in theNi78region

Borzov

2005

Phys. Rev. C

View full text Add to dashboard Cite

A systematic study of the total β-decay half-lives and β-delayed neutron emission probabilities is performed. The β-strength function is treated within a self-consistent density-functional + continuum-quasiparticle-randomphase-approximation framework including the Gamow-Teller and first-forbidden transitions. The experimental total β-decay half-lives for the Ni isotopes with A 76 are described satisfactorily. The half-lives predicted from A = 70 up to A = 86 reveal fairly regular A behavior which results from simultaneous account for the Gamow-Teller and first-forbidden transitions. For Z ≈ 28 nuclei, a suppression of the delayed neutron emission probability is found when the N = 50 neutron closed shell is crossed and the neutron excess becomes more than one major shell. The effect originates from the high-energy first-forbidden transitions to the states outside the Q β -B n window in the daughter nuclei.

show abstract

Section: β-Strength Functionmentioning

confidence: 99%

“…The method to include the ph continuum for the T = 1 excitations of superfluid nuclei [18,20] is similar to the one for T = 0 excitations [21]. It is based on the exact treatment of the pairing in "valence λ space" (µ τ − ξ < ε λ < µ τ + ξ ), where µ τ are the neutron and proton chemical potentials.…”

Section: β-Strength Functionmentioning

confidence: 99%

β-delayed neutron emission in theNi78region

Borzov

2005

Phys. Rev. C

View full text Add to dashboard Cite

show abstract

“…The allowed transitions for the charged-current (anti)neutrino scatterings are treated fully microscopically within the cQRPA approximation (Borzov et al 1995;Borzov & Goriely 2000) and on grounds of the ETFSI ground state description (Aboussiret al 1995). The Gamow-Teller (GT) strength function accounts for the transitions to the daughter nucleus ground and lowlying states, to the GT resonance (GTR) and to the particle continuum region above the GTR.…”

Section: The Production Of 138 La By Neutrino Capturesmentioning

confidence: 99%

The puzzle of the synthesis of the rare nuclide $\mathsf{^{138}}$La

Goriely

Arnould

Borzov

et al. 2001

A&A

View full text Add to dashboard Cite

Abstract. The calculations of the p-process in the O/Ne layers of Type II supernovae are quite successful in reproducing the solar system content of p-nuclides. They predict, however, a significant underproduction of the rare odd-odd nuclide 138 La. A model for the explosion of a 25 M star with solar metallicity is used to suggest that νe-captures on 138 Ba may well be its most efficient production mechanism. The responsibility of an inadequate prediction of the 138 La and 139 La photodisintegration rates in the too low production of 138 La is also examined quantitatively. A detailed discussion of the theoretical uncertainties in these rates suggest that the required rate changes are probably too high to be fully plausible. Their measurement would be most welcome. They would help disentangling the relative contributions of thermonuclear and neutrino processes to the 138 La production.Key words. nuclear reactions -nucleosynthesis -solar system: general IntroductionThe odd-odd neutron-deficient heavy nuclides 138 La and isomeric 180 Ta m are among the rarest solar system species (no information exists for other locations), with 138La/ 139 La ≈ 10 −3 and 180 Ta m / 181 Ta ≈ 10 −4 . In spite of their scarcity, their origin has long been a puzzle. As initially claimed by Prantzos et al. (1990) and confirmed by Rayet et al. (1995; hereafter RAHPN), 180 Ta m appears to be a natural product of the p-process in the O/Ne-rich layers of Type II supernovae (SNII). In contrast, 138 La is underproduced in all p-process calculations performed so far (e.g. Fig. 1 of Arnould et al. 2001).In view of the low 138 La abundance, it has been attempted to explain its production by non-thermonuclear processes involving either stellar energetic particles (Audouze 1970) or neutral current neutrino-induced transmutations (Woosley et al. 1990). The former mechanism is predicted not to be efficient enough, while the latter is found by Woosley et al. (1990) to be able to overproduce the solar 138 La/ 139 La ratio by a factor of about 50. This prediction has to be taken with some care, however, especially in view of the qualitative nature of the evaluation.In a one-dimensional Z = Z M = 25 M SNII model, 138 La is predicted to be produced only at peak temperatures around 2.4 ± 0.1 × 10 9 K (Arnould et al. 2001) from a subtle balance between its main production by 139 La (γ , n) 138 La and its main destruction by 138 La (γ , n) 137 La . The resulting abundances cannot account for the solar system 138 La amount. The same conclusion holds for all the stars in the 13 ≤ M/M ≤ 25Send offprint requests to: S. Goriely, e-mail: sgoriely@astro.ulb.ac.be examined by RAHPN. This situation might of course just result from inadequate astrophysics and/or nuclear physics inputs. On the astrophysics side, one might incriminate an uncertain prediction of the evolution of the thermodynamic conditions of the 138 La producing layers during the explosion. Modifying these conditions is unlikely, however, to cure the 138 La underproduction. For any astrophysically pl...

show abstract

“…Such a cQRPA approach to describing charge-exchange excitations has been developed in Refs. [12,13].…”

Section: Introductionmentioning

confidence: 99%

Description of double β decay within the continuum quasiparticle random-phase approximation

Rodin

Faessler

2008

Phys. Rev. C

View full text Add to dashboard Cite

A method to calculate the nuclear double beta decay (2νββ and 0νββ) amplitudes within the continuum quasiparticle random phase approximation (cQRPA) is formulated. Calculations of the ββ transition amplitudes within the cQRPA are performed for 76 Ge, 100 Mo and 130 Te. A rather simple nuclear Hamiltonian consisting of a phenomenological mean field and a zero-range residual particle-hole and particle-particle interaction is used. The calculated 2νββ amplitudes are almost unaffected when the single-particle continuum is taken into account, whereas we find a regular suppression of the 0νββ amplitudes that can be associated with additional ground-state correlations owing to collective states in the continuum. It is expected that inclusion of nucleon pairing in the single-particle continuum will somewhat compensate this suppression.

show abstract

Gamow-Teller strength functions of superfluid odd-A nuclei and neutrino capture reactions

Cited by 54 publications

References 42 publications

β-delayed neutron emission in theNi78region

β-delayed neutron emission in theNi78region

The puzzle of the synthesis of the rare nuclide $\mathsf{^{138}}$La

Description of double β decay within the continuum quasiparticle random-phase approximation

Contact Info

Product

Resources

About