A. N. Kuchera

Area of research

Nuclear and High Energy Physics · Radiation

Research interest

Research topics from publications: ON THE MEASUREMENT OF THE13C(α,n)16OS-FACTOR AT NEGATIVE ENERGIES AND ITS INFLUENCE ON THEs-PROCESS; Constraining the 6.05 MeV0+and 6.13 MeV3−Cascade Transitions in the<mml:math xmlns:mml="http:/; Measurement of the−3 keVResonance in the ReactionC13(α,</mml:; New measurement of theαasymptotic normalization coefficient of the1/2+state inO<mml:; Observation of a Near-Threshold Proton Resonance in B11; ANASEN: The array for nuclear astrophysics and structure with exotic nuclei; α-cluster asymptotic normalization coefficients for nuclear astrophysics; STUDIES OF EXOTIC NUCLEI AT THE RESOLUT FACILITY OF FLORIDA STATE UNIVERSITY; Clustering in non-self-conjugate nuclei10Be and18O; Clustering in Non-Self-Conjugate Nuclei. Representative work: The 13C(α, n)16O reaction is the neutron source for the main component of the s-process, responsible for the production of most of the nuclei in the mass range 90 ≲ A ≲ 208. This reaction takes place inside the helium-burning shell of asymptotic giant branch stars, at temperatures ≲ 108 K, corresponding to an energy interval where the 13C(α, n)16O reaction is effective in the range of 140–230 keV. In this regime, the astrophysical S(E)-factor is dominated by the −3 keV sub-threshold resonance due to the 6.356 MeV level in 17O, giving rise to a steep increase in the S-factor. Its contribution is still controversial as extrapolations, e.g., through the R-matrix and indirect techniques such as The $^{12}\mathrm{C}(\ensuremath{\alpha},\ensuremath{\gamma})^{16}\mathrm{O}$ reaction plays a fundamental role in astrophysics and needs to be known with accuracy better than 10%. Cascade $\ensuremath{\gamma}$ transitions through the excited states of $^{16}\mathrm{O}$ are contributing to the uncertainty. We constrained the contribution of the ${0}^{+}$ (6.05 MeV) and ${3}^{\ensuremath{-}}$ (6.13 MeV) cascade transitions by measuring the asymptotic normalization coefficients for these states using the $\ensuremath{\alpha}$-transfer reaction ${}^{6}\mathrm{L}\mathrm{i}({}^{12}\mathrm{C},d{)}^{16}\mathrm{O}$ at sub-Coulomb energy. The contribution of the $0{}^{+}$ and ${3}^{\ensuremath{-}}$ c

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