arXiv subjects

K. I. Tursunmakhatov

Publications and source records attributed to K. I. Tursunmakhatov.

6 recordsLinked to original sources

arXiv2024

Reply to the "Comments to the paper "Detailed study of the astrophysical direct capture reaction $^{6}{\rm Li}(p, γ)^{7}{\rm Be}$ in ..." " by S.B. Dubovichenko, A.S. Tkachenko, R. Ya. Kezerashvili, arXiv:2401.04281 (2024)

The differences in potential models used in our work and in the original paper of the authors of the Comment are discussed. The neglecting of simple rules of reaction calculations is shown as a possible origin of the defect in the temperature dependence of the reaction rates in the work of the authors of the Comment.

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arXiv2023

Detailed study of the astrophysical direct capture reaction $^{6}{\rm Li}(p, γ)^{7}{\rm Be}$ in a potential model approach

The astrophysical $S$ factor and reaction rates of the direct capture process $^{6}$Li(p,$γ)^{7}$Be are estimated within a two-body single-channel potential model approach. Central potentials of the Gaussian-form in the $^2P_{3/2}$ and $^2P_{1/2}$ waves are adjusted to reproduce the binding energies and the empirical values of the asymptotic normalization coefficients (ANC) for the $^7$Be(3/2$^-$) ground and $^7$Be(1/2$^-$) excited bound states, respectively. The parameters of the potential in the most important $^2S_{1/2}$ scattering channel were fitted to reproduce the empirical phase shifts from the literature and the low-energy astrophysical $S$ factor of the LUNA collaboration. The obtained results for the astrophysical $S$ factor and the reaction rates are in a very good agreement with available experimental data sets. The numerical estimates reproduce not only the absolute values, but also the energy and temperature dependence of the $S$ factor and reaction rates of the LUNA collaboration, respectively. The estimated $^{7}{\rm Li/H}$ primordial abundance ratio $(4.67\pm 0.04 )\times 10^{-10}$ is well consistent with recent BBN result of $(4.72\pm 0.72) \times 10^{-10}$ after the Planck observation.

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arXiv2020

Dispersion (asymptotic) theory of charged particle transfer reactions at low energies and nuclear astrophysics: II. the asymptotic normalization coefficients and their nuclear-astrophysical application

Within the asymptotic theory proposed by authors R. Yarmukhamedov and K.I. Tursunmakhatov [Phys. Rev. C (submitted 2019)] for the peripheral sub- and above-barrier transfer $A$($x$, $y$)$B$ reaction in the three-body ($A$, $a$ and $y$) model ($ x$= $y$ + $a$ and $B$= $A$ + $a$, and $ a$ is a transferred particle), the analysis of the experimental angular distributions of the differential cross sections is performed for the peripheral proton and triton transfer ${\rm{^9Be(^{10}B,\,^9Be)^{10}B}}$, ${\rm{^{16}O(^3He}},\,d{\rm{)^{17}F}}$ and ${\rm{^{19}F(}}p,\,α{\rm{)^{16}O}}$ reactions at above-and sub-barrier projectile energies, respectively. New estimates and their uncertainties are obtained for magnitudes of the asymptotic normalization coefficients (respective the nuclear vertex constants) for ${\rm{^9Be}} \,+p \to\,{\rm{^{10}B}}$, ${\rm{^{16}O}} \,+\,p \to\, {\rm{^{17}F}}$ and ${\rm{^{16}O}} \,+\,t\to{\rm{^{19}F}}$. They are applied for calculations of the astrophysical $S$ factors for the nuclear-astrophysical ${\rm{^9Be(}}p,\,γ{\rm{)^{10}B}} $, ${\rm{^{16}O(}}p,\,γ{\rm{)^{17}F}}$ and ${\rm{^{19}F(}}p,\,α{\rm{)^{16}O)}}$ reactions at thermonuclear energies. New values and their uncertainties are obtained for the astrophysical $S$ factors at stellar energies.

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arXiv2020

Dispersion (asymptotic) theory of charged particle transfer reactions at low energies and nuclear astrophysics: I. the "non-dramatic" case

A new dispersion (asymptotic) theory is proposed for the peripheral sub- and above-barrier charged particle transfer $A(x,y)B$ reaction in the three-body ($A$, $a$ and $y$) model where $ x= y +a$ and $B=A+a$, and $ a$ is a transferred particle. It is based on the combination of the dispersion theory and the conventional DWBA method. The explicit forms have been derived for the exact three-body pole amplitude and differential cross section in which the contribution of the three-body ($A$, $a$ and $y$) Coulomb dynamics of the transfer mechanism in the peripheral partial amplitudes, corresponding to partial waves with $l_i>>1$, is taken into account correctly. For the specific peripheral proton and triton transfer reactions, the comparative analysis of the peripheral partial amplitudes at $l_i>>1$ , which correspond to the one-step pole and exact three-body pole amplitudes as well as those of the "post"-approximation and the post form of the conventional DWBA, is performed with each other. It shows the absolute inapplicability of the "post"-approximation usually applied for getting an information about specific asymptotic normalization coefficients being astrophysical interest.

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arXiv2018

Asymptotic theory of charged particle transfer reactions at low energies and nuclear astrophysics

A new asymptotic theory is proposed for the peripheral sub- and above-barrier transfer $A$($x$, $y$)$B$ reaction within the three-body ($A$, $a$ and $y$) model, where $ x$= $y$ + $a$, $B$= $A$ + $a$ and $ a$ is a transferred particle. In the asymptotic theory, the allowance of the contribution of the three-body ($A$, $a$ and $y$) Coulomb dynamics of the transfer mechanism to the peripheral partial amplitudes for the partial wave $l_i>>$ 1 and of the Coulomb-nuclear distorted effects in the entrance and exit channels is done in a correct manner within the framework of the dispersion theory and the conventional distorted-wave Born approximation (DWBA), respectively. It is shown that the proposed asymptotic theory makes it possible to test the accuracy of taking into account the the three-body Coulomb dynamics of the transfer mechanism in the modified DWBA. The results of the analysis of the differential cross sections of the specific proton and triton transfer reactions at above- and sub-barrier energies are presented. New estimates and their uncertainties are obtained for values of the asymptotic normalization coefficients for ${\rm{^9Be}} \,+p \to\,{\rm{^{10}B}}$, ${\rm{^{11}B}}\,+\,p\to\,{\rm{^{12}C}}$, ${\rm{^{16}O}} \,+\,p \to\, {\rm{^{17}F}}$ and ${\rm{^{19}F}}\to\, {\rm{^{16}O}} \,+\,t$ as well as for the direct astrophysical $S$ factors at stellar energy of the radiative capture ${\rm{^9Be(}}p,\,γ{\rm{)^{10}B}} $, ${\rm{^{11}B(}}p,\,γ{\rm{)^{12}C}} $ and ${\rm{^{16}O(}}p,\,γ{\rm{)^{17}F}}$ reactions.

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arXiv2008

Determination of the 3He+alpha\to 7Be asymp. normalization coefficients (nucl. vertex constants) and their application for extrapolation of the 3He(alpha,gamma)7Be astroph. S-factors to the solar energy region

A new analysis of the precise experimental astrophysical $S$-factors for the direct capture $^3He(α,γ)^7{\rm {Be}}$ reaction [B.S. Nara Singh et al., Phys.Rev.Lett. {\bf 93} (2004) 262503; D. Bemmerer et al., Phys.Rev.Lett. {\bf 97} (2006) 122502; F.Confortola et al., Phys.Rev. {\bf C 75} (2007) 065803 and T.A.D.Brown et al., Phys.Rev. {\bf C 76} (2007) 055801] populating to the ground and first excited states of $^7{\rm Be}$ is carried out based on the modified two - body potential approach in which the direct astrophysical $S$-factor, $S_{34}(E)$, is expressed in terms of the asymptotic normalization constants for $^3{\rm {He}}+α\to ^7{\rm {Be}}$ and two additional conditions are involved to verify the peripheral character of the reaction under consideration. The Woods--Saxon potential form is used for the bound ($α+^3{\rm {He}}$)- state and the $^3{\rm {He}}α$- scattering wave functions. New estimates are obtained for the "indirectly measured", values of the asymptotic normalization constants (the nuclear vertex constants) for $^3{\rm {He}}+α\to^7{\rm {Be}}(g.s.)$ and $^3{\rm {He}}+α\to^7{\rm {Be}}(0.429 MeV)$ as well as the astrophysical $S$-factors $S_{34}(E)$ at E$\le$ 90 keV, including $E$=0. The values of asymptotic normalization constants have been used for getting information about the $α$-particle spectroscopic factors for the mirror ($^7Li^7{\rm {Be}}$)-pair.

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