Stellar reaction rate for {sup 22}Mg+p->{sup 23}Al from the asymptotic normalization coefficient in the mirror nuclear system {sup 22}Ne+n->{sup 23}Ne

Journal Article · Mon Mar 15 00:00:00 EDT 2010 · Physical Review. C, Nuclear Physics

DOI:https://doi.org/10.1103/PHYSREVC.81.035802· OSTI ID:21388893

Al-Abdullah, T ^[1]; Carstoiu, F ^[2]; Chen, X; Clark, H L; Fu, C; Gagliardi, C A; Lui, Y -W; Mukhamedzhanov, A; Tabacaru, G; Tokimoto, Y; Trache, L; Tribble, R E ^[1]

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1. Cyclotron Institute, Texas A and M University, College Station, Texas 77843 (United States)
2. National Institute for Physics and Nuclear Engineering 'Horia Hulubei', R-76900 Bucharest-Magurele (Romania)

The production of {sup 22}Na in ONe novae can be influenced by the {sup 22}Mg(p,gamma){sup 23}Al reaction. To investigate this reaction rate at stellar energies, we have determined the asymptotic normalization coefficient (ANC) for {sup 22}Mg+p->{sup 23}Al through measurements of the ANCs in the mirror nuclear system {sup 22}Ne+n->{sup 23}Ne. The peripheral neutron-transfer reactions {sup 13}C({sup 12}C,{sup 13}C){sup 12}C and {sup 13}C({sup 22}Ne,{sup 23}Ne){sup 12}C were studied. The identical entrance and exit channels of the first reaction make it possible to extract independently the ground-state ANC in {sup 13}C. Our experiment gives C{sub p{sub 1/2}}{sup 2}({sup 13}C)=2.24+-0.11 fm{sup -1}, which agrees with the value obtained from several previous measurements. The weighted average for all the obtained C{sub p{sub 1/2}}{sup 2} is 2.31+-0.08 fm{sup -1}. This value is adopted to be used in obtaining the ANCs in {sup 23}Ne. The differential cross sections for the reaction {sup 13}C({sup 22}Ne,{sup 23}Ne){sup 12}C leading to the J{sup {pi}}=5/2{sup +} and 1/2{sup +} states in {sup 23}Ne have been measured at 12 MeV/u. Optical model parameters for use in the DWBA calculations were obtained from measurements of the elastic scatterings {sup 22}Ne+{sup 13}C and {sup 22}Ne+{sup 12}C. The extracted ANC for the ground state in {sup 23}Ne, C{sub d{sub 5/2}}{sup 2}=0.86+-0.08+-0.12 fm{sup -1}, is converted to its corresponding value in {sup 23}Al using mirror symmetry to give C{sub d{sub 5/2}}{sup 2}({sup 23}Al)=(4.63+-0.77)x10{sup 3} fm{sup -1}. The astrophysical S factor S(0) for the {sup 22}Mg(p,gamma) reaction was determined to be 0.96+-0.11 keV b. The consequences for nuclear astrophysics are discussed.

• OSTI ID: 21388893
• Journal Information: Physical Review. C, Nuclear Physics, Vol. 81, Issue 3; Other Information: DOI: 10.1103/PhysRevC.81.035802; (c) 2010 The American Physical Society; ISSN 0556-2813
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
ALUMINIUM 23
ASYMPTOTIC SOLUTIONS
CARBON 12
CARBON 13
DIFFERENTIAL CROSS SECTIONS
DWBA
ELASTIC SCATTERING
GAMMA DECAY
GROUND STATES
KEV RANGE
MAGNESIUM 22
MEV RANGE
MIRROR NUCLEI
NEON 22
NEON 23
NEUTRON REACTIONS
NEUTRON TRANSFER
NUCLEAR REACTIONS
OPTICAL MODELS
PROTON REACTIONS
REACTION KINETICS
SODIUM 22
STARS
SYMMETRY
ALKALINE EARTH ISOTOPES
ALUMINIUM ISOTOPES
APPROXIMATIONS
BARYON REACTIONS
BETA DECAY RADIOISOTOPES
BETA-MINUS DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
BORN APPROXIMATION
CALCULATION METHODS
CARBON ISOTOPES
CHARGED-PARTICLE REACTIONS
CROSS SECTIONS
DECAY
ENERGY LEVELS
ENERGY RANGE
EVEN-EVEN NUCLEI
EVEN-ODD NUCLEI
HADRON REACTIONS
ISOMERIC TRANSITION ISOTOPES
ISOTOPES
KINETICS
LIGHT NUCLEI
MAGNESIUM ISOTOPES
MATHEMATICAL MODELS
MATHEMATICAL SOLUTIONS
MILLISECONDS LIVING RADIOISOTOPES
NANOSECONDS LIVING RADIOISOTOPES
NEON ISOTOPES
NUCLEAR DECAY
NUCLEI
NUCLEON REACTIONS
ODD-EVEN NUCLEI
ODD-ODD NUCLEI
RADIOISOTOPES
SCATTERING
SECONDS LIVING RADIOISOTOPES
SODIUM ISOTOPES
STABLE ISOTOPES
YEARS LIVING RADIOISOTOPES