Investigation of the 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mmultiscripts><mml:mi mathvariant="normal">N</mml:mi><mml:mprescripts /><mml:none /><mml:mn>14</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mo>)</mml:mo></mml:mrow><mml:mmultiscripts><mml:mi mathvariant="normal">O</mml:mi><mml:mprescripts /><mml:none /><mml:mn>15</mml:mn></mml:mmultiscripts></mml:math>
 reaction and its impact on the CNO cycle

Frentz, B.; Aprahamian, A.; Boeltzig, A.; Borgwardt, Tyler; Clark, Adam M.; deBoer, R. J.; Gilardy, G.; Hanhardt, M.; Henderson, S. L.; Howard, Kevin; Kadlecek, Thomas; Liu, Q.; Macon, K. T.; Moylan, Shane; Reingold, Craig; Robertson, Daniel; Seymour, C.; Strauss, S.; Strieder, F.; Kolk, B. Vande; Wiescher, M.

doi:10.1103/physrevc.106.065803

Cited by 6 publications

(2 citation statements)

References 49 publications

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“…The results coincide with those reported in Refs. [13,15,23,25,26,34] within limits of errors. The spectroscopic factors and physics of the single particle strength distribution in nuclei are connected.…”

Section: E1 E1mentioning

confidence: 99%

“…Furthermore, the normalization parameters (spectroscopic factor) were too low for the listed transitions considered in these calculations. Li et al [25] measured the excitation function as well as angular distributions of the two transitions in 15 O. They employed the multi-channel R-matrix analysis and computed the astrophysical S-factors for the transitions to the ground and fourth excited states of 15 O.…”

Section: Introductionmentioning

confidence: 99%

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Radiative capture of proton through the ¹⁴N(p,γ)¹⁵O reaction at low energy

Irgaziev,

Kabir,

Nabi

2024

Chinese Phys. C

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The CNO cycle is the main source of energy in stars more massive than our Sun. It defines the energy production and the duration contributes in determining the lifetime of massive stars. The cycle is an important tool for the determination of the age of globular clusters. Radiative capture p + 14N →15O + γ, at energies of astrophysical interest, is one of the important processes in the CNO cycle. In this project, we apply a potential model to describe both non-resonant and resonant reactions in the channels where radiative capture occurs through electric E1 transitions. We employed the R-matrix method to describe the reactions going via M1 resonant transitions, when it was not possible to correctly reproduce the experimental data by a potential model. The partial components of the astrophysical S-factor were calculated for all possible electric and magnetic dipole transitions in 15O. The linear extrapolated S-factor at zero energy (S(0)) is in good agreement with earlier reported values for all types of transitions considered in this work. Based on the value of the total astrophysical S-factor, depending on the collision energy, we calculate the nuclear reaction rates for p + 14N →15O + γ. The computed rates are in good agreement with the results of the NACRE II Collaboration.

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