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Title: Astrophysical S-factors for the p+16O and n+16O captures from the analysis of 16O(d,n)17F and 16O(d,p)17O transfer reactions

Abstract

Coupled reaction channels calculations were performed for the 16O(d,n)17F and 16O(d,p)17O transfer reactions for the ground and first excited states at several energies from Elab=2.29 MeV up to 3.27 MeV. A strong polarization effect between the entrance channel and the transfer, 16O(d,n)17F (1/2+,0.495) and 16O(d,n)17O (1/2+0.87), channels was observed. This polarization effect had to be taken into account to all orders for obtaining realistic spectroscopic factors from these reactions. The 16O(p,{gamma})17F and 16O(n,{gamma})17O direct captures were calculated using the Asymptotic Normalization Coefficients (ANC) values from these transfer reactions analysis. The astrophysical S-factors were compared to measurements. The Maxwellian-averaged neutron capture cross section at kT=30 keV was 22(3){mu}barn.

Authors:
; ; ;  [1];  [2];  [3]
  1. Departamento de Fisica Nuclear, Instituto de Fisica da Universidade de Sao Paulo, CP 66318, 05315-970 Sao Paulo SP (Brazil)
  2. Departamento de Fisica, Instituto Superior Tecnico, Taguspark, 2780-990 Porto Salvo (Portugal)
  3. (Spain)
Publication Date:
OSTI Identifier:
21054808
Resource Type:
Journal Article
Resource Relation:
Journal Name: AIP Conference Proceedings; Journal Volume: 884; Journal Issue: 1; Conference: 6. Latin American symposium on nuclear physics and applications, Iguazu (Argentina), 3-7 Oct 2005; Other Information: DOI: 10.1063/1.2710573; (c) 2007 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
73 NUCLEAR PHYSICS AND RADIATION PHYSICS; ASTROPHYSICS; ASYMPTOTIC SOLUTIONS; CAPTURE; CROSS SECTIONS; DEUTERON REACTIONS; DEUTERONS; EXCITED STATES; FLUORINE 17; KEV RANGE; MEV RANGE; NEUTRON REACTIONS; NEUTRONS; OXYGEN 16; OXYGEN 16 TARGET; OXYGEN 17; POLARIZATION; PROTON REACTIONS; PROTONS; SPECTROSCOPIC FACTORS; TRANSFER REACTIONS

Citation Formats

Assuncao, M., Lichtenthaeler, R., Guimaraes, V., Lepine-Szily, A., Moro, A. M., and Departamento de FAMN, Universidad de Sevilla, Apdo. 1065, E-41080 Sevilla. Astrophysical S-factors for the p+16O and n+16O captures from the analysis of 16O(d,n)17F and 16O(d,p)17O transfer reactions. United States: N. p., 2007. Web. doi:10.1063/1.2710573.
Assuncao, M., Lichtenthaeler, R., Guimaraes, V., Lepine-Szily, A., Moro, A. M., & Departamento de FAMN, Universidad de Sevilla, Apdo. 1065, E-41080 Sevilla. Astrophysical S-factors for the p+16O and n+16O captures from the analysis of 16O(d,n)17F and 16O(d,p)17O transfer reactions. United States. doi:10.1063/1.2710573.
Assuncao, M., Lichtenthaeler, R., Guimaraes, V., Lepine-Szily, A., Moro, A. M., and Departamento de FAMN, Universidad de Sevilla, Apdo. 1065, E-41080 Sevilla. Mon . "Astrophysical S-factors for the p+16O and n+16O captures from the analysis of 16O(d,n)17F and 16O(d,p)17O transfer reactions". United States. doi:10.1063/1.2710573.
@article{osti_21054808,
title = {Astrophysical S-factors for the p+16O and n+16O captures from the analysis of 16O(d,n)17F and 16O(d,p)17O transfer reactions},
author = {Assuncao, M. and Lichtenthaeler, R. and Guimaraes, V. and Lepine-Szily, A. and Moro, A. M. and Departamento de FAMN, Universidad de Sevilla, Apdo. 1065, E-41080 Sevilla},
abstractNote = {Coupled reaction channels calculations were performed for the 16O(d,n)17F and 16O(d,p)17O transfer reactions for the ground and first excited states at several energies from Elab=2.29 MeV up to 3.27 MeV. A strong polarization effect between the entrance channel and the transfer, 16O(d,n)17F (1/2+,0.495) and 16O(d,n)17O (1/2+0.87), channels was observed. This polarization effect had to be taken into account to all orders for obtaining realistic spectroscopic factors from these reactions. The 16O(p,{gamma})17F and 16O(n,{gamma})17O direct captures were calculated using the Asymptotic Normalization Coefficients (ANC) values from these transfer reactions analysis. The astrophysical S-factors were compared to measurements. The Maxwellian-averaged neutron capture cross section at kT=30 keV was 22(3){mu}barn.},
doi = {10.1063/1.2710573},
journal = {AIP Conference Proceedings},
number = 1,
volume = 884,
place = {United States},
year = {Mon Feb 12 00:00:00 EST 2007},
month = {Mon Feb 12 00:00:00 EST 2007}
}
  • Astrophysical S-factors of (p, n) reactions on {sup 99}Ru, {sup 100}Ru, {sup 101}Ru, and {sup 102}Ru were derived from the sum of experimental isomeric and ground states cross sections measured in the incident proton energy range of 5-9 MeV. They were compared with Hauser-Feshbach statistical model predictions of the NON-SMOKER code. Good agreement was found in the majority of cases. Reaction rates were derived up to 8.7 GK stellar temperature by combining experiment and theory.
  • The cross section of the radiative proton capture reaction on the drip line nucleus {sup 12}N was investigated using the asymptotic normalization coefficient (ANC) method. We have used the {sup 14}N({sup 12}N,{sup 13}O){sup 13}C proton transfer reaction at 12 MeV/nucleon to extract the ANC for {sup 13}O{yields}{sup 12}N+p and calculate from it the direct component of the astrophysical S factor of the {sup 12}N(p,{gamma}){sup 13}O reaction. The optical potentials used and the distorted-wave Born approximation analysis of the proton transfer reaction are discussed. For the entrance channel, the optical potential was inferred from an elastic scattering measurement carried out atmore » the same time as the transfer measurement. From the transfer, we determined the square of the ANC, C{sub p{sub 1/2}}{sup 2}({sup 13}O{sub g.s.})=2.53{+-}0.30 fm{sup -1}, and hence a value of 0.33(4) keV b was obtained for the direct astrophysical S factor at zero energy. Constructive interference at low energies between the direct and resonant captures leads to an enhancement of S{sub total}(0)=0.42(6) keV b. The {sup 12}N(p,{gamma}){sup 13}O reaction was investigated in relation to the evolution of hydrogen-rich massive Population III stars, for the role that it may play in the hot pp-chain nuclear burning processes, possibly occurring in such objects.« less
  • The reaction cross section of the radiative proton capture on the drip line nucleus {sup 12}N was studied at the Cyclotron Institute at Texas A and M University. We have employed the indirect Asymptotic Normalization Coefficient method to determine the direct radiative component of the astrophysical S-factor of the {sup 12}N(p,{gamma}){sup 13}O reaction. A value of 0.31(5) keV{center_dot}b was found at zero energy. Interference between direct and resonant captures leads to a further enhancement of a factor of two. The reaction was investigated in relation to the evolution of hydrogen-rich massive objects, Population III stars, because of the role thatmore » it may play in the hot pp chain nuclear burning processes occurring in such stars.« less
  • At very low energies of astrophysical interest, the {sup 7}Be({ital p},{gamma}){sup 8}B reaction is almost totally peripheral. Consequently, the overall normalization of the cross section for this reaction is defined by the asymptotic normalization coefficient of the bound-state wave function of {sup 8}B in the two-body channel {sup 7}Be+{ital p}. The reaction {sup 7}Be({sup 3}He,{ital d}){sup 8}B is suggested as a tool to measure this asymptotic normalization coefficient thereby allowing one to define the absolute value of the astrophysical factor, {ital S}{sub 17}(0), for the {sup 7}Be({ital p},{gamma}){sup 8}B reaction.