Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=8cm,clip]{figure1.eps} \end{figure}$ Figure 1: Absolute-magnitude (in blue filter) distributions of various types of SNe from Richardson et al. (2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure2.eps} \end{figure}$ Figure 2: The SN distribution in explosion energies $\Psi (E_{51})$ converted from the Mb-distribution presented in Fig. 1. The high energy part of the distribution is presented separately.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure3.eps} \end{figure}$ Figure 3: Total (SUM) proton spectrum (in relative units) generated by 7 different types of SNe with parameters from Table 1. The contribution of each SNe type is presented separately.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure6.eps} \end{figure}$ Figure 6: The average mass number $<\ln~A>$ of CRs in the KASCADE experiment (full squares) and in the calculations: full line - main variant, dashed line - variant when CRs from SNIIn are enriched by heavy nuclei.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure8.eps} \end{figure}$ Figure 8: The integral distributions $W(>\!\!E_{51})$ for different variants of calculations in comparison with the "real SNe'' distribution from Hamuy (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure9.eps} \end{figure}$ Figure 9: All-particle spectra calculated with different variants of the $W(>\!\!E_{51})$ functions presented in Fig. 8 (lines) in comparison with the experimental all-particle spectrum (stars) averaged over many EAS experiments by Hoerandel (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{figure1.eps} \end{figure}$	Figure 1: Absolute-magnitude (in blue filter) distributions of various types of SNe from Richardson et al. (2002).
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure2.eps} \end{figure}$	Figure 2: The SN distribution in explosion energies $\Psi (E_{51})$ converted from the Mb-distribution presented in Fig. 1. The high energy part of the distribution is presented separately.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure3.eps} \end{figure}$	Figure 3: Total (SUM) proton spectrum (in relative units) generated by 7 different types of SNe with parameters from Table 1. The contribution of each SNe type is presented separately.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure4.eps} \end{figure}$	Figure 4: Spectra of different cosmic ray nuclei.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure5.eps} \end{figure}$	Figure 5: The contributions of various types of SN explosions into all-particle spectrum.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure6.eps} \end{figure}$	Figure 6: The average mass number $<\ln~A>$ of CRs in the KASCADE experiment (full squares) and in the calculations: full line - main variant, dashed line - variant when CRs from SNIIn are enriched by heavy nuclei.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure7.eps} \end{figure}$	Figure 7: The dependence of the knee location on maximal energy of SN explosions.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure8.eps} \end{figure}$	Figure 8: The integral distributions $W(>\!\!E_{51})$ for different variants of calculations in comparison with the "real SNe'' distribution from Hamuy (2003).
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{figure9.eps} \end{figure}$	Figure 9: All-particle spectra calculated with different variants of the $W(>\!\!E_{51})$ functions presented in Fig. 8 (lines) in comparison with the experimental all-particle spectrum (stars) averaged over many EAS experiments by Hoerandel (2003).
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