Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig1.ps}\end{figure}$ Figure 1: Bolometric magnitude at maximum as function of time step $\Delta \log ~ t$ . Time derivatives are approximated with Eq. (19) ( open circles) or Eq. (20) ( filled circles). The extrapolation to vanishingly small time step is shown ( star) as are $\pm$ 0.05 mag error bands.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig2.ps}\end{figure}$ Figure 2: Comparison of bolometric light curves. The light curve obtained with the 3-D Monte Carlo code ( filled circles) compared to that obtained from the moment equations ( solid line). The corresponding ${\gamma }$ -ray deposition curves are also plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig3.ps}\end{figure}$ Figure 3: Light curve residuals. The differences between the bolometric light curves plotted in Fig. 2 as a function of elapsed time t. Residuals for 3-D MC calculations with 100³ ( filled circles) and 20³ ( open circles) grids are shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1656fig4.ps}\end{figure}$ Figure 4: Energy fractions as functions of elapsed time t. Quantities plotted are $E_{\gamma }$ , the integrated energy released by radioactive decays, $E_{\infty }$ , the integrated energy emitted to $\infty$ , W, the work done on the expanding ejecta, and $E_{\rm R}$ , the radiant energy stored in the ejecta. The unit of energy is $E_{{\rm tot}}$ - see Eq. (3) - so that $E_{\gamma }(\infty ) = 1$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig5.ps}\end{figure}$ Figure 5: Residence times $\Delta t = t_{{\rm esc}} - t_{\gamma }$ plotted against $t_{{\rm esc}}$ . Escaping r packets ( open circles) and ${\gamma }$ -packets ( filled circles) are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig1.ps}\end{figure}$	Figure 1: Bolometric magnitude at maximum as function of time step $\Delta \log ~ t$ . Time derivatives are approximated with Eq. (19) ( open circles) or Eq. (20) ( filled circles). The extrapolation to vanishingly small time step is shown ( star) as are $\pm$ 0.05 mag error bands.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig2.ps}\end{figure}$	Figure 2: Comparison of bolometric light curves. The light curve obtained with the 3-D Monte Carlo code ( filled circles) compared to that obtained from the moment equations ( solid line). The corresponding ${\gamma }$ -ray deposition curves are also plotted.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig3.ps}\end{figure}$	Figure 3: Light curve residuals. The differences between the bolometric light curves plotted in Fig. 2 as a function of elapsed time t. Residuals for 3-D MC calculations with 100³ ( filled circles) and 20³ ( open circles) grids are shown.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{1656fig5.ps}\end{figure}$	Figure 5: Residence times $\Delta t = t_{{\rm esc}} - t_{\gamma }$ plotted against $t_{{\rm esc}}$ . Escaping r packets ( open circles) and ${\gamma }$ -packets ( filled circles) are indicated.
Open with DEXTER