Speakers
Mr
Juan Carlos Morales-Rivera
(Universidad Autónoma del Estado de México)Prof.
Tatyana Belyaeva
(Universidad Autonoma del Estado de Mexico)
Description
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{\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy}
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\TITLE{Breakup of $^{8}B$ on $^{58}Ni$ at energies below the Coulomb barrier and the astrophysical $S_{17}(0)$ factor revisited}\\[3mm]
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\AUTHORS{\underline{J. C. Morales-Rivera}$^{1,2}$, T. L. Belyaeva$^1$, P. Amador-Valenzuela$^{2}$, E. F. Aguilera$^{2}$, \\
E. Martinez-Quiroz$^{2}$ and J. J. Kolata$^{3}$ }
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\AFFILIATION{1}{Universidad Aut\'onoma del Estado de M\'exico, C. P. 50000, Toluca, M\'exico}
\AFFILIATION{2}{Depto. de Aceleradores, Instituto Nacional de Investigaciones Nucleares, A. P. 18-1027, C. P. 11801
M\'exico, D. F., M\'exico}
\AFFILIATION{3}{Physics Department, University of Notre Dame, Notre Dame, Indiana, 46556, USA}
}
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\centerline{Contact email: {\it carlosmoriv@hotmail.com}}
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Calculations of breakup and direct proton transfer by Continuum-Discretized Coupled Channels (CDCC) were made for the $^{8}B$+$^{58}Ni$ system at energies around the Coulomb barrier $E_{B_{c.m.}}=20.8 ~MeV$. For the $^{7}Be$-target interaction, we used a Semimicroscopic Optical Model that combines microscopic calculations of the mean-field double folding potential and a phenomenological construction of the dynamical polarization potential (DPP) [1]. The DPP parameters were fitting to reproduce the elastic scattering angular distributions of $^{8}B$ on $^{58}Ni$ at various energies [2] (Fig. 1), the $^{8}B$ breakup angular distributions at $25.75 ~MeV$ [3], and the energy dependence of the fusion cross sections for the $^{8}B$+$^{58}Ni$ system [2]. We also study the effect of different proton-core and -target interactions on the breakup angular distributions in comparison with the previous calculations [4]. Preliminary value of the spectroscopy factor for $^{8}B$ $\rightarrow$ $^{7}Be+p$ vertices $S_{exp}=1.0$ was deduced from comparison with the data [5]. It allowed us to estimate the asymptotic normalization coefficient, $C^{2}=0.49 ~fm^{-1}$, and the astrophysical $S_{17}(0)$ factor to be $18.8 ~eV ~b$, which are in good accordance with the published results [5].
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\begin{figure}[h]
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\includegraphics[width=0.4\textwidth]{Dis_ang}
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\caption{Comparison of the experimental data [2] and calculated elastic scattering angular distributions for the $^{8}B$+$^{58}Ni$ system.}
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\textit{Work partially supported by CONACYT, Mexico.}
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{\small
\noindent [1] S. A. Goncharov and A. Izadpanah, Phys. At. Nucl. \textbf{70} (2007) pp. 18-28.
\noindent [2] E. F. Aguilera \textit{et al}., Phys. Rev. C \textbf{79}, 021601(R) (2009).
\noindent [3] J. J. Kolata \textit{et al}., Phys. Rev. C \textbf{63}, 024616 (2001).
\noindent [4] T. L. Belyaeva \textit{et at}., Phys. Rev. C \textbf{80}, 064617 (2009)
\noindent [5] O. R. Tojiboev \textit{et al}., Phys. Rev. C. \textbf{94}, 054616 (2016).
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Primary author
Mr
Juan Carlos Morales-Rivera
(Universidad Autónoma del Estado de México)
Co-authors
Dr
Eli F. Aguilera
(ININ)
Dr
Enrique Martinez-Quiroz
(ININ)
Dr
James Kolata
(University of Notre Dame)
Dr
Paulina Amador-Valenzuela
(ININ)
Prof.
Tatyana Belyaeva
(Universidad Autonoma del Estado de Mexico)
