624 research outputs found
Neutrinoless decay nuclear matrix elements in an isotopic chain
We analyze nuclear matrix elements (NME) of neutrinoless double beta decay
calculated for the Cadmium isotopes. Energy density functional methods
including beyond mean field effects such as symmetry restoration and shape
mixing are used. Strong shell effects are found associated to the underlying
nuclear structure of the initial and final nuclei. Furthermore, we show that
NME for two-neutrino double beta decay evaluated in the closure approximation,
, display a constant proportionality with respect to
the Gamow-Teller part of the neutrinoless NME, . This
opens the possibility of determining the matrix
elements from Gamow-Teller strength functions. Finally, the
interconnected role of deformation, pairing, configuration mixing and shell
effects in the NMEs is discussed
Supernova neutrinos and nucleosynthesis
Observations of metal-poor stars indicate that at least two different
nucleosynthesis sites contribute to the production of r-process elements. One
site is responsible for the production of light r-process elements Z<~50 while
the other produces the heavy r-process elements. We have analyzed recent
observations of metal-poor stars selecting only stars that are enriched in
light r-process elements and poor in heavy r-process elements. We find a strong
correlation between the observed abundances of the N=50 elements (Sr, Y and Zr)
and Fe. It suggest that neutrino-driven winds from core-collapse supernova are
the main site for the production of these elements. We explore this possibility
by performing nucleosynthesis calculations based on long term Boltzmann
neutrino transport simulations. They are based on an Equation of State that
reproduces recent constrains on the nuclear symmetry energy. We predict that
the early ejecta is neutron-rich with Ye ~ 0.48, it becomes proton rich around
4 s and reaches Ye = 0.586 at 9 s when our simulation stops. The
nucleosynthesis in this model produces elements between Zn and Mo, including
92Mo. The elemental abundances are consistent with the observations of the
metal-poor star HD 12263. For the elements between Ge and Mo, we produce mainly
the neutron-deficient isotopes. This prediction can be confirmed by
observations of isotopic abundances in metal-poor stars. No elements heavier
than Mo (Z=42) and no heavy r-process elements are produced in our
calculations.Comment: 18 pages, 5 figures, submitted to J. Phys. G: Nucl. Part. Phys.
(Focus issue "Nucleosynthesis and the role of neutrinos", ed. Baha Balantekin
and Cristina Volpe
Neutrino-nucleus reactions and their role for supernova dynamics and nucleosynthesis
The description of nuclear reactions induced by supernova neutrinos has
witnessed significant progress during the recent years. At the energies and
momentum transfers relevant for supernova neutrinos neutrino-nucleus cross
sections are dominated by allowed transitions, however, often with
non-negligible contributions from (first) forbidden transitions. For several
nuclei allowed Gamow-Teller strength distributions could be derived from
charge-exchange reactions and from inelastic electron scattering data.
Importantly the diagonalization shell model has been proven to accurately
describe these data and hence became the appropriate tool to calculate the
allowed contributions to neutrino-nucleus cross sections for supernova
neutrinos. Higher multipole contributions are usually calculated within the
framework of the Quasiparticle Random Phase Approximation, which describes the
total strength and the position of the giant resonances quite well.
This manuscript reviews the recent progress achieved in calculating
supernova-relevant neutrino-nucleus cross sections and discusses its
verification by data. Moreover, the review summarizes also the impact which
neutrino-nucleus reactions have on the dynamics of supernovae and on the
associated nucleosynthesis. These include the absorption of neutrinos by nuclei
(the inverse of nuclear electron capture which is the dominating
weak-interaction process during collapse), inelastic neutrino-nucleus
scattering and nuclear de-excitation by neutrino-pair emission. We also discuss
the role of neutrino-induced reactions for the recently discovered
process, for the r-process and for the neutrino process, for which
neutrino-nucleus reactions have the largest impact. Finally, we briefly review
neutrino-nucleus reactions important for the observation of supernova neutrinos
by earthbound detectors. (Abridged)Comment: 77 pages, 29 figures, 4 tables, submitted to Progress in Particle and
Nuclear Physic
Systematic study of infrared energy corrections in truncated oscillator spaces
We study the convergence properties of nuclear binding energies and
two-neutron separation energies obtained with self-consistent mean-field
calculations based on the Hartree-Fock-Bogolyubov (HFB) method with Gogny-type
effective interactions. Owing to lack of convergence in a truncated working
basis, we employ and benchmark one of the recently proposed infrared energy
correction techniques to extrapolate our results to the limit of an infinite
model space. We also discuss its applicability to global calculations of
nuclear masses.Comment: 12 pages, 12 figure
Neutrino–nucleus reactions and nuclear structure
The methods used in the evaluation of the neutrino–nucleus cross section are reviewed. Results are shown for a variety of targets of practical importance. Many of the described reactions are accessible in future experiments with neutrino sources from the pion and muon decays at rest, which might be available at the neutron spallation facilities. Detailed comparison between the experimental and theoretical results would establish benchmarks needed for verification and/or parameter adjustment of the nuclear models. Having a reliable tool for such calculation is of great importance in a variety of applications, e.g. the neutrino oscillation studies, detection of supernova neutrinos, description of the neutrino transport in supernovae and description of the r-process nucleosynthesis
Neutrino Nucleosynthesis of radioactive nuclei in supernovae
We study the neutrino-induced production of nuclides in explosive supernova
nucleosynthesis for progenitor stars with solar metallicity and initial main
sequence masses between 15 M and 40 M. We improve previous
investigations i) by using a global set of partial differential cross sections
for neutrino-induced charged- and neutral-current reactions on nuclei with
charge numbers and ii) by considering modern supernova neutrino
spectra which have substantially lower average energies compared to those
previously adopted in neutrino nucleosynthesis studies. We confirm the
production of Li, B, La, and Ta by neutrino
nucleosynthesis, albeit at slightly smaller abundances due to the changed
neutrino spectra. We find that for stars with a mass smaller than 20 M,
F is produced mainly by explosive nucleosynthesis while for higher mass
stars it is produced by the process. We also find that neutrino-induced
reactions, either directly or indirectly by providing an enhanced abundance of
light particles, noticeably contribute to the production of the radioactive
nuclides Na and Al. Both nuclei are prime candidates for
gamma-ray astronomy. Other prime targets, Ti and Fe, however, are
insignificantly produced by neutrino-induced reactions. We also find a large
increase in the production of the long-lived nuclei Nb and Tc due
to charged-current neutrino capture.Comment: 6 pages, 2 figures, 2 table
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