2,161 research outputs found
Upper Limit on the molecular resonance strengths in the C+C fusion reaction
Carbon burning is a crucial process for a number of important astrophysical
scenarios. The lowest measured energy is around E=2.1 MeV, only
partially overlapping with the energy range of astrophysical interest. The
currently adopted reaction rates are based on an extrapolation which is highly
uncertain because of potential resonances existing in the unmeasured energy
range and the complication of the effective nuclear potential. By comparing the
cross sections of the three carbon isotope fusion reactions,
C+C, C+C and C+C, we have
established an upper limit on the molecular resonance strengths in
C+C fusion reaction. The preliminary results are presented
and the impact on nuclear astrophysics is discussed.Comment: 4 pages, 3 figures, FUSION11 conference proceedin
Determination of Omega_b From Big Bang Nucleosynthesis in the Presence of Regions of Antimatter
Production of regions of antimatter in the early universe is predicted in
many baryogenesis models. Small scale antimatter regions would annihilate
during or soon after nucleosynthesis, affecting the abundances of the light
elements. In this paper we study how the acceptable range in Omega_b changes in
the presence of antimatter regions, as compared to the standard big bang
nucleosynthesis. It turns out that it is possible to produce at the same time
both a low 4He value (Y_p < 0.240) and a low D/H value (D/H < 4e-5), but
overproduction of 7Li is unavoidable at large Omega_b.Comment: 9 pages, PRD version, ref. 6 correcte
Role of break-up processes in fusion enhancement of drip-line nuclei at energies below the Coulomb barrier
We carry out realistic coupled-channels calculations for
Be + Pb reaction in order to discuss the effects of break-up
of the projectile nucleus on sub-barrier fusion.
We discretize in energy the particle continuum states, which are associated
with the break-up process, and construct the coupling form factors to these
states on a microscopic basis.
The incoming boundary condition is employed in solving coupled-channels
equations, which enables us to define the flux for complete fusion inside the
Coulomb barrier. It is shown that complete fusion cross sections are
significantly enhanced due to the couplings to the continuum states compared
with the no coupling case at energies below the Coulomb barrier, while they are
hindered at above barrier energies.Comment: RevTex, 3 pages, 5 figure
Alpha-decay branching ratios of near-threshold states in <sup>19</sup>Ne and the astrophysical rate of <sup>15</sup> O(α, γ )<sup>19</sup>Ne
The 15O(α,γ)19Ne reaction is one of two routes for breakout from the hot CNO cycles into the rp process in accreting neutron stars. Its astrophysical rate depends critically on the decay properties of excited states in 19Ne lying just above the 15O + α threshold. We have measured the α-decay branching ratios for these states using the p(21lNe,t)19Ne reaction at 43 MeV/u.</p
Influence of nuclear structure on sub-barrier hindrance in Ni+Ni fusion
Fusion-evaporation cross sections for Ni+Ni have been measured
down to the 10 nb level. For fusion between two open-shell nuclei, this is the
first observation of a maximum in the -factor, which signals a strong
sub-barrier hindrance. A comparison with the Ni+Ni,
Ni+Ni, and Ni+Ni systems indicates a strong
dependence of the energy where the hindrance occurs on the stiffness of the
interacting nuclei.Comment: Submitted to Phys. Rev. Lett. 4 pages, 3 figure
Quantum Tunneling in Nuclear Fusion
Recent theoretical advances in the study of heavy ion fusion reactions below
the Coulomb barrier are reviewed. Particular emphasis is given to new ways of
analyzing data, such as studying barrier distributions; new approaches to
channel coupling, such as the path integral and Green function formalisms; and
alternative methods to describe nuclear structure effects, such as those using
the Interacting Boson Model. The roles of nucleon transfer, asymmetry effects,
higher-order couplings, and shape-phase transitions are elucidated. The current
status of the fusion of unstable nuclei and very massive systems are briefly
discussed.Comment: To appear in the January 1998 issue of Reviews of Modern Physics. 13
Figures (postscript file for Figure 6 is not available; a hard copy can be
requested from the authors). Full text and figures are also available at
http://nucth.physics.wisc.edu/preprints
Alpha-decay branching ratios of near-threshold states in 19Ne and the astrophysical rate of 15O(alpha,gamma)19Ne
The 15O(alpha,gamma)19Ne reaction is one of two routes for breakout from the
hot CNO cycles into the rp process in accreting neutron stars. Its
astrophysical rate depends critically on the decay properties of excited states
in 19Ne lying just above the 15O + alpha threshold. We have measured the
alpha-decay branching ratios for these states using the p(21Ne,t)19Ne reaction
at 43 MeV/u. Combining our measurements with previous determinations of the
radiative widths of these states, we conclude that no significant breakout from
the hot CNO cycle into the rp process in novae is possible via
15O(alpha,gamma)19Ne, assuming current models accurately represent their
temperature and density conditions
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