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33 та иш

Иш: ANC and SF of bound states in 15N→14C+p, 16O→15N+p, 19F→18O+p, 32S→31P+p

  1. Asymptotic normalization coefficients for<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow/><mml:mrow><mml:mn>10</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">B</mml:mi><mml:mrow><mml:msup><mml:mrow><mml:mo>→</mml:mo></mml:mrow><mml:mrow><mml:mn>9</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">Be</mml:mi><mml:mo>+</mml:mo><mml:mi>p</mml:mi></mml:math>

    A. M. Mukhamedzhanov, H. L. Clark, C. A. Gagliardi +9

    Мақола199729 иқтибос
    ABI

  2. Local and global nucleon optical models from 1 keV to 200 MeV

    A. J. Koning, J. P. Delaroche

    Мақола200212 иқтибос
    ABI

  3. Spectroscopic factors and asymptotic normalization coefficients for<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mn>0</mml:mn><mml:mi>p</mml:mi></mml:mrow></mml:math>-shell nuclei: Recent updates

    N. K. Timofeyuk

    Мақола201310 иқтибос
    ABI

  4. Determination of nuclear vertex constants (asymptotic normalization coefficients) for the virtual decays 3He → d + p and 17F → 16O + p and their use for extrapolating astrophysical S-factors of the radiative proton capture by the deuteron and the 16O nucleus at very low energies

    S. V. Artemov, S. B. Igamov, K. I. Tursunmakhatov +1

    МақолаNuclear physics research studiesBulletin of the Russian Academy of Sciences Physics20098 иқтибос
    ABI

  5. Global deuteron optical model potential for the energy range up to 183 MeV

    Haixia An, Chonghai Cai

    Мақола20068 иқтибос
    ABI

  6. Asymptotic normalization coefficients for <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mmultiscripts><mml:mi>Be</mml:mi><mml:mprescripts/><mml:none/><mml:mn>7</mml:mn></mml:mmultiscripts><mml:mspace width="0.16em"/><mml:mo>+</mml:mo><mml:mspace width="0.16em"/><mml:mi>p</mml:mi><mml:mo>→</mml:mo><mml:mmultiscripts><mml:mi mathvariant="normal">B</mml:mi><mml:mprescripts/><mml:none/><mml:mn>8</mml:mn></mml:mmultiscripts></mml:mrow></mml:math> from the peripheral <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mmultiscripts><mml:mi>Be</mml:mi><mml:mprescripts/><mml:none/><mml:mn>7</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mi>d</mml:mi><mml:mo>,</mml:mo><mml:mi>n</mml:mi><mml:mo>)</mml:mo><mml:mmultiscripts><mml:mi mathvariant="normal">B</mml:mi><mml:mprescripts/><mml:none/><mml:mn>8</mml:mn></mml:mmultiscripts></mml:mrow></mml:math> reaction and their astrophysical application

    O. R. Tojiboev, R. Yarmukhamedov, S. V. Artemov +1

    МақолаNuclear physics research studiesPhysical review. C20168 иқтибос
    ABI

  7. Spectroscopic factors from one-proton stripping reactions on sd-shell nuclei: experimental measurements and shell-model calculations

    J. Vernotte, G. Berrier-Ronsin, J. Kalifa +2

    Мақола19946 иқтибос
    ABI

  8. Overlap functions, spectroscopic factors, and asymptotic normalization coefficients generated by a shell-model source term

    N. K. Timofeyuk

    Мақола20105 иқтибос
    ABI

  9. Late-time neutron diffusion and nucleosynthesis in a post-QCD inhomogeneous Omega(b) = 1 universe

    Robert Malaney, William A. Fowler

    Мақола19884 иқтибос
    ABI

  10. Global optical model potential for<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>A</mml:mi><mml:mo>=</mml:mo><mml:mn>3</mml:mn></mml:mrow></mml:math>projectiles

    D. Y. Pang, P. Roussel-Chomaz, H. Savajols +2

    Мақола20094 иқтибос
    ABI

  11. New astrophysical<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>S</mml:mi></mml:mrow></mml:math>factor for the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">N</mml:mi><mml:mprescripts/><mml:none/><mml:mrow><mml:mn>15</mml:mn></mml:mrow></mml:mmultiscripts></mml:math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mo stretchy="false">(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:mrow></mml:math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">O</mml:mi><mml:mprescripts/><mml:none/><mml:mrow><mml:mn>16</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>reaction via the asymptotic normalization coefficient (ANC) method

    A. M. Mukhamedzhanov, P. Bém, V. Burjan +17

    Мақола20082 иқтибос
    ABI

  12. Elastic scattering of 9–13 MeV vector polarized deuterons

    J. Lohr, W. Haeberli

    Мақола19742 иқтибос
    ABI

  13. Optical model potential of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>A</mml:mi><mml:mo>=</mml:mo><mml:mn>3</mml:mn></mml:mrow></mml:math>projectiles for<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mn>1</mml:mn><mml:mi>p</mml:mi></mml:mrow></mml:math>-shell nuclei

    D. Y. Pang, W. M. Dean, A. M. Mukhamedzhanov

    Мақола20152 иқтибос
    ABI

  14. Transfer reaction code with nonlocal interactions

    L. J. Titus, A. Ross, F. M. Nunes

    Мақола20162 иқтибос
    ABI

  15. <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mo>(</mml:mo><mml:mi>d</mml:mi><mml:mo>,</mml:mo><mml:mi>n</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math> proton-transfer reactions on <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi>Be</mml:mi><mml:mprescripts/><mml:none/><mml:mn>9</mml:mn></mml:mmultiscripts><mml:mo>,</mml:mo><mml:mo> </mml:mo><mml:mmultiscripts><mml:mi mathvariant="normal">B</mml:mi><mml:mprescripts/><mml:none/><mml:mn>11</mml:mn></mml:mmultiscripts><mml:mo>,</mml:mo><mml:mo> </mml:mo><mml:mmultiscripts><mml:mi mathvariant="normal">C</mml:mi><mml:mprescripts/><mml:none/><mml:mn>13</mml:mn></mml:mmultiscripts><mml:mo>,</mml:mo><mml:mo> </mml:mo><mml:mmultiscripts><mml:mi mathvariant="normal">N</mml:mi><mml:mprescripts/><mml:none/><mml:mrow><mml:mn>14</mml:mn><mml:mo>,</mml:mo><mml:mn>15</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>, and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi mathvariant="normal">F</mml:mi><mml:mprescripts/><mml:none/><mml:mn>19</mml:mn></mml:mmultiscripts></mml:math> and spectroscopic factors at <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msub><mml:mi>E</mml:mi><mml:mi>d</mml:mi></mml:msub><mml:mo>=</mml:mo><mml:mn>16</mml:mn><mml:mspace width="0.16em"/><mml:mi>MeV</mml:mi></mml:mrow></mml:math>

    M. Febbraro, F.D. Becchetti, R. O. Torres-Isea +4

    Мақола20172 иқтибос
    ABI

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