$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig1.eps} \end{figure}$ Figure 1: Stellar ¹⁸⁷Os(n, $\gamma$ )¹⁸⁸Os rate as a function of the temperature for 3 different prescriptions of the width fluctuation correction and without any.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig2.eps} \end{figure}$ Figure 2: Comparison of MOST (crosses) or TALYS (circles) radiative neutron capture rates with experimental data above Ca (Bao et al. 2000) at the temperature $T=3 \times 10^8$ K.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig3.eps} \end{figure}$ Figure 3: Ratio of MOST to TALYS radiative neutron capture rates for all Sn (crosses) and Pb (circles) isotopes at T=10⁹ K as a function of the neutron number N.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig4.eps} \end{figure}$ Figure 4: Ratio of MOST to TALYS radiative neutron capture rates for all nuclei with $16 \le Z \le 83$ at T=10⁹ K as a function of the neutron number N.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig5.eps} \end{figure}$ Figure 5: Radiative neutron capture cross section for ¹¹⁶Sn ( top) and ¹⁴⁰Sn ( bottom) with and without including the pre-equilibrium processes as a function of energy.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig6.eps} \end{figure}$ Figure 6: Ratio of the radiative neutron capture ( top) and photoneutron ( bottom) rates obtained with and without including the pre-equilibrium processes for all Sn isotopes at 3 different temperatures T₉.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=6.8cm,clip]{8825fig7.eps} \end{figure}$ Figure 7: Representation in the (N,Z) plane, as given by the legend, of the value of the critical temperature at which the Maxwellian-averaged (n,2n) rate becomes faster than the (n, $\gamma$ ) rate, i.e. r_n=1.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig1.eps} \end{figure}$	Figure 1: Stellar ¹⁸⁷Os(n, $\gamma$ )¹⁸⁸Os rate as a function of the temperature for 3 different prescriptions of the width fluctuation correction and without any.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig2.eps} \end{figure}$	Figure 2: Comparison of MOST (crosses) or TALYS (circles) radiative neutron capture rates with experimental data above Ca (Bao et al. 2000) at the temperature $T=3 \times 10^8$ K.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig3.eps} \end{figure}$	Figure 3: Ratio of MOST to TALYS radiative neutron capture rates for all Sn (crosses) and Pb (circles) isotopes at T=10⁹ K as a function of the neutron number N.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig4.eps} \end{figure}$	Figure 4: Ratio of MOST to TALYS radiative neutron capture rates for all nuclei with $16 \le Z \le 83$ at T=10⁹ K as a function of the neutron number N.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig5.eps} \end{figure}$	Figure 5: Radiative neutron capture cross section for ¹¹⁶Sn ( top) and ¹⁴⁰Sn ( bottom) with and without including the pre-equilibrium processes as a function of energy.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{8825fig6.eps} \end{figure}$	Figure 6: Ratio of the radiative neutron capture ( top) and photoneutron ( bottom) rates obtained with and without including the pre-equilibrium processes for all Sn isotopes at 3 different temperatures T₉.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,height=6.8cm,clip]{8825fig7.eps} \end{figure}$	Figure 7: Representation in the (N,Z) plane, as given by the legend, of the value of the critical temperature at which the Maxwellian-averaged (n,2n) rate becomes faster than the (n, $\gamma$ ) rate, i.e. r_n=1.
Open with DEXTER