985 research outputs found
Relativistic continuum-continuum coupling in the dissociation of halo nuclei
A relativistic coupled-channels theory for the calculation of dissociation
cross sections of halo nuclei is developed. A comparison with non-relativistic
models is done for the dissociation of B projectiles. It is shown that
neglecting relativistic effects leads to seizable inaccuracies in the
extraction of the astrophysical S-factor for the proton+beryllium radiative
capture reaction.Comment: 4 pages, 2 figures, version accepted for publication at Physics
Review Letter
The reaction 13C(alpha,n)16O: a background for the observation of geo-neutrinos
The absolute cross section of the C(,n)O reaction has
been measured at E = 0.8 to 8.0 MeV with an overall accuracy of 4%.
The precision is needed to subtract reliably a background in the observation of
geo-neutrinos, e.g. in the KamLAND detector.Comment: LaTex file, 13 pages including 3 ps figures. Any request to
[email protected]. Phys. Rev . C, to appea
Theoretical photo-disintegration of O
The photodisintegration of O is predicted to be dominated by 2
excitation in the vicinity of the -particle threshold.
The reaction rates of C(,)O are expected to be
determined from this reaction.Comment: 3 pages, 2 figures, Proceedings of Nuclei in the Cosmos (NIC-XIV).
19-24 June 2016, Niigata, Japa
Proton Threshold States in the 22Na(p,gamma)23Mg Reaction and Astrophysical Implications
Proton threshold states in 23Mg are important for the astrophysically
relevant proton capture reaction 22Na(p,gamma)23Mg. In the indirect
determination of the resonance strength of the lowest states, which were not
accessible by direct methods, some of the spin-parity assignments remained
experimentally uncertain. We have investigated these states with Shell Model,
Coulomb displacement, and Thomas-Ehrman shift calculations. From the comparison
of calculated and observed properties we relate the lowest relevant resonance
state at E=7643 keV to an excited 3/2+ state in accordance with a recent
experimental determination by Jenkins et al.. From this we deduce significantly
improved values for the 22Na(p,gamma)23Mg reaction rate at stellar temperatures
below T_9=0.1K.Comment: 8 pages, 4 figures, 6 table
Study of the 12C+12C fusion reactions near the Gamow energy
The fusion reactions 12C(12C,a)20Ne and 12C(12C,p)23Na have been studied from
E = 2.10 to 4.75 MeV by gamma-ray spectroscopy using a C target with ultra-low
hydrogen contamination. The deduced astrophysical S(E)* factor exhibits new
resonances at E <= 3.0 MeV, in particular a strong resonance at E = 2.14 MeV,
which lies at the high-energy tail of the Gamow peak. The resonance increases
the present non-resonant reaction rate of the alpha channel by a factor of 5
near T = 8x10^8 K. Due to the resonance structure, extrapolation to the Gamow
energy E_G = 1.5 MeV is quite uncertain. An experimental approach based on an
underground accelerator placed in a salt mine in combination with a high
efficiency detection setup could provide data over the full E_G energy range.Comment: 4 Pages, 4 figures, accepted for publication in Phys. Rev. Let
Notes on the Pollination of Some Liliaceae and a Few Other Plants
It will not be necessary in this connection to refer to the literature. This may be obtained from such works as Herman \u27Mueller and Darcy W. Thompson. In the identification of insects help was obtained from Prof. Osborn and Miss Beach
LUNA: Nuclear Astrophysics Deep Underground
Nuclear astrophysics strives for a comprehensive picture of the nuclear
reactions responsible for synthesizing the chemical elements and for powering
the stellar evolution engine. Deep underground in the Gran Sasso laboratory the
cross sections of the key reactions of the proton-proton chain and of the
Carbon-Nitrogen-Oxygen (CNO) cycle have been measured right down to the
energies of astrophysical interest. The salient features of underground nuclear
astrophysics are summarized here. The main results obtained by LUNA in the last
twenty years are reviewed, and their influence on the comprehension of the
properties of the neutrino, of the Sun and of the Universe itself are
discussed. Future directions of underground nuclear astrophysics towards the
study of helium and carbon burning and of stellar neutron sources in stars are
pointed out.Comment: Invited review, submitted to Annu. Rev. Nucl. Part. Scienc
Imaginary-time method for radiative capture reaction rate
We propose a new computational method for astrophysical reaction rate of
radiative capture process. In the method, an evolution of a wave function is
calculated along the imaginary-time axis which is identified as the inverse
temperature. It enables direct evaluation of reaction rate as a function of
temperature without solving any scattering problem. The method is tested for
two-body radiative capture reaction, , showing that it gives identical results to that calculated by the
ordinary procedure. The new method will be suited for calculation of
triple-alpha radiative capture rate for which an explicit construction of the
scattering solution is difficult.Comment: 8 pages, 7 figure
Nuclear masses, deformations and shell effects
We show that the Liquid Drop Model is best suited to describe the masses of
prolate deformed nuclei than of spherical nuclei. To this end three Liquid Drop
Mass formulas are employed to describe nuclear masses of eight sets of nuclei
with similar quadrupole deformations. It is shown that they are able to fit the
measured masses of prolate deformed nuclei with an RMS smaller than 750 keV,
while for the spherical nuclei the RMS is, in the three cases, larger than 2000
keV. The RMS of the best fit of the masses of semi-magic nuclei is also larger
than 2000 keV. The parameters of the three models are studied, showing that the
surface symmetry term is the one which varies the most from one group of nuclei
to another. In one model, isospin dependent terms are also found to exhibit
strong changes. The inclusion of shell effects allows for better fits, which
continue to be better in the prolate deformed nuclei regionComment: 10 pages, 8 tables, Proc. of the XXXIV Nuclear Physics Symposium,
January 4-7 2011, Cocoyoc, Morelos, Mexico. IOP Journal of Physics:
Conference Series (in press
Solving the two-center nuclear shell-model problem with arbitrarily-orientated deformed potentials
A general new technique to solve the two-center problem with
arbitrarily-orientated deformed realistic potentials is demonstrated, which is
based on the powerful potential separable expansion method. As an example,
molecular single-particle spectra for C + C Mg are
calculated using deformed Woods-Saxon potentials. These clearly show that
non-axial symmetric configurations play a crucial role in molecular resonances
observed in reaction processes for this system at low energy
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