The elastic scattering 7Be + p at low energies: implications on the 7Be(p, γ)8Be S-factor

2003 ◽  
Vol 719 ◽  
pp. C300-C303 ◽  
Author(s):  
C. Angulo ◽  
P. Descouvemont ◽  
M. Cogneau ◽  
M. Couder ◽  
M. Gaelens ◽  
...  
Keyword(s):  
Elastic Scattering ◽  
S Factor ◽  
Low Energies

scholarly journals S-factor of 14N(α,γ)18F reaction at low-energies

2018 ◽  
Vol 9 ◽  
pp. 1116-1119
Author(s):  
H. Khalili
Keyword(s):  
S Factor ◽  
Low Energies

Astrophysical S factor of the radiative 4He12C-capture reaction at low energies

2011 ◽  
Vol 75 (11) ◽  
pp. 1517-1522 ◽  
Author(s):  
S. B. Dubovichenko ◽  
A. V. Dzhazairov-Kakhramanov
Keyword(s):  
Capture Reaction ◽  
S Factor ◽  
Low Energies

scholarly journals Experimental measurement of the 12C+16O fusion cross sections at astrophysical energies

2018 ◽  
Vol 178 ◽  
pp. 04008
Author(s):  
X. Fang ◽  
W. P. Tan ◽  
M. Beard ◽  
R. J. deBoer ◽  
G. Gilardy ◽  
...  
Keyword(s):  
Cross Sections ◽  
Center Of Mass ◽  
Model Calculations ◽  
Center Of Mass Energy ◽  
Pure Graphite ◽  
S Factor ◽  
Hpge Detectors ◽  
Low Energies ◽  
The University

The total cross sections of the 12C+16O fusion have been experimentally determined at low energies to investigate the role of this reaction during late stellar evolution burning phases. A high-intensity oxygen beam was produced by the 5MV pelletron accelerator at the University of Notre Dame impinging on a thick ultra-pure graphite target. Protons and γ-rays were measured simultaneously in the center-of-mass energy range from 3.64 to 5.01 MeV, using strip silicon and HPGe detectors. Statistical model calculations were employed to interpret the experimental results. A new broad resonance-like structure is observed for the 12C+16O reaction, and a decreasing trend of its S-factor towards low energies is found.

scholarly journals Fusion and elastic scattering of 6Li + 58Ni at low energies

2017 ◽  
Vol 163 ◽  
pp. 00001 ◽  
Author(s):  
Elí F. Aguilera ◽  
Paulina Amador-Valenzuela ◽  
Enrique Martinez-Quiroz ◽  
David Lizcano ◽  
Araceli Garcia-Flores ◽  
...  
Keyword(s):  
Elastic Scattering ◽  
Low Energies

scholarly journals Astrophysical S-factor of the radiative proton capture on 14C at low energies

2014 ◽  
Vol 29 (24) ◽  
pp. 1450125 ◽  
Author(s):  
Sergey Dubovichenko ◽  
Nasurlla Burtebaev ◽  
Albert Dzhazairov-Kakhramanov ◽  
Dilshod Alimov
Keyword(s):  
Ground State ◽  
Cluster Model ◽  
Phase Shift Analysis ◽  
Potential Cluster Model ◽  
Proton Capture ◽  
Position Location ◽  
Capture Reaction ◽  
Shift Analysis ◽  
S Factor ◽  
Low Energies

The phase shift analysis for position location of the [Formula: see text] resonance at 1.5 MeV was carried out on the basis of the known experimental measurements of the excitation functions of the p14 C elastic scattering at four angles from 90° to 165° and more than 100 energy values in the range from 600–800 keV to 2200–2400 keV. Also, the possibility to describe the available experimental data on the astrophysical S-factor for the proton capture reaction on 14 C to the ground state (GS) of 15 N at astrophysical energies was considered in the frame of modified potential cluster model (MPCM).

scholarly journals Fusion hindrance in light and heavy systems

2019 ◽  
Vol 223 ◽  
pp. 01041
Author(s):  
Giovanna Montagnoli
Keyword(s):  
Theoretical Work ◽  
Heavy Ion ◽  
General Phenomenon ◽  
Quantitative Evidence ◽  
Coupled Channels ◽  
S Factor ◽  
Low Energies ◽  
Show Evidence ◽  
Heavy Ion Fusion ◽  
Transfer Channels

The phenomenon of hindrance in sub-barrier heavy-ion fusion has been confirmed by several experimentalevidences and it is now recognised as a general phenomenon of heavy-ion fusion process. In many cases the signature of fusion hindrance lies in the trend of the logarithmic slope of the excitation function and of the S factor at low energies. The comparison with stadard Coupled-Channels calculations is a more quantitative evidence for its existence. In many medium-heavy systems the hindrance effect has been recognised with different features depending on the various couplings to the inelastic and transfer channels. Different theoretical appro ches have been proposed to explain the hindrance but the underlying physics is still a matter of debate. Hindrance is observed in light systems, independent of the sign of the fusion Q-value, with different features. In the case of the 12C + 30Si system the effect is smallbut it is clearly observed. Near-by cases show evidence for systematic behaviours. A very recent experiment has concerned the lighter case 12C + 24Mg where hindrance shows up clearly, because a maximum of the S factor appears already at a relatively high cross section σ=1.6mb. The consequences for the dynamics of stellar evolution have to be clarified by further experimental and theoretical work.

scholarly journals Breakup, fusion, and elastic scattering analysis of the8B +58Ni system at low energies with the continuum-discretized coupled channels method

2014 ◽  
Vol 66 ◽  
pp. 03008 ◽  
Author(s):  
T. L. Belyaeva ◽  
P. Amador-Valenzuela ◽  
E. F. Aguilera ◽  
E. Martinez-Quiroz ◽  
J. J. Kolata
Keyword(s):  
Elastic Scattering ◽  
Coupled Channels ◽  
Low Energies ◽  
The Continuum

scholarly journals Asymptotic normalization coefficient for α+d →6Li from the peripheral direct capture d(α,γ)6 reaction and the astrophysical S factor at Big Bang energies

2020 ◽  
Vol 227 ◽  
pp. 02016
Author(s):  
K.I. Tursunmakhatov ◽  
R. Yarmukhamedov ◽  
S.B. Igamov
Keyword(s):  
Big Bang ◽  
Asymptotic Normalization ◽  
Direct Capture ◽  
Asymptotic Normalization Coefficient ◽  
S Factor ◽  
Low Energies

The results of the analysis of the new experimental astrophysical S factors Sexp24(E) [D. Trezzi, et al., Astropart. Phys. 89, 57 (2017)] and those measured earlier [R. G. Robertson, et al., Phys. Rev. Lett. 47, 1867 (1981)] for the nuclear-astrophysical d(α,γ)6Li reaction directly measured at extremely low energies E, are presented. New estimates and their uncertainties have been obtained for values of the asymptotic normalization coefficient for α + γ → 6Li and for the direct astrophysical S factors at Big Bang energies.

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