Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{3051fig1.eps} \end{figure}$ Figure 1: HR diagram of the program Be stars in terms of the BCD ( $\lambda _1,D$ ) parameters. Each curvilinear quadrilateral represents a MK spectral type-luminosity class group. The vertical strips demarcate the spectral types, which are given in the abscissa. The luminosity classes corresponding to the horizontal strips are marked in the quadrilaterals on the right side of the diagram.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3051fig2.eps} \end{figure}$ Figure 2: Model $(\lambda _1,D)$ parameters against the rate $\Omega /\Omega _{\rm {c}}$ for different unperturbed pairs $(T_{\rm eff},\log g)$ and several aspect angles i.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3051fig3.eps} \end{figure}$ Figure 3: Functions F_T and F_G for $\tau /\tau _{\rm MS} = 0.5$ and two stellar masses.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3051fig4.eps} \end{figure}$ Figure 4: Evolutionary tracks for different initial velocities $V_{\rm o}$ . " ${\it dotted}$ '' lines are for evolutionary tracks with $V_{\rm o} = 0$ km s^-1; " ${\it full}$ '' lines are for $V_{\rm o} = 300$ km s^-1; " ${\it dashed}$ '' lines correspond to $V_{\rm o} = f(M)$ so that $V_{\rm o} = 340$ km s^-1 at $3~M_{\odot}$ and 420 km s^-1 for $30~M_{\odot}$ .
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{3051fig5.eps} \end{figure}$ Figure 5: HR diagrams of the studied Be stars. a) Apparent ( $\log L/L_{\odot},\log T_{\rm eff}$ ) with evolutionary tracks without rotation. b) Surface averaged ( $\log L/L_{\odot},\log T_{\rm eff}$ ) and evolutionary tracks with initial an equatorial rotation velocity $V_{\rm o} = 300$ km s^-1 for all masses.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{3051fig6.eps} \end{figure}$ Figure 6: Age ratios $\tau /\tau _{\rm MS}$ of the studied Be stars against the mass. a) Parameters derived using evolutionary tracks without rotation; b) parameters derived using evolutionary tracks with rotation.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3051fig1.eps} \end{figure}$	Figure 1: HR diagram of the program Be stars in terms of the BCD ( $\lambda _1,D$ ) parameters. Each curvilinear quadrilateral represents a MK spectral type-luminosity class group. The vertical strips demarcate the spectral types, which are given in the abscissa. The luminosity classes corresponding to the horizontal strips are marked in the quadrilaterals on the right side of the diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{3051fig2.eps} \end{figure}$	Figure 2: Model $(\lambda _1,D)$ parameters against the rate $\Omega /\Omega _{\rm {c}}$ for different unperturbed pairs $(T_{\rm eff},\log g)$ and several aspect angles i.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3051fig3.eps} \end{figure}$	Figure 3: Functions F_T and F_G for $\tau /\tau _{\rm MS} = 0.5$ and two stellar masses.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3051fig4.eps} \end{figure}$	Figure 4: Evolutionary tracks for different initial velocities $V_{\rm o}$ . " ${\it dotted}$ '' lines are for evolutionary tracks with $V_{\rm o} = 0$ km s^-1; " ${\it full}$ '' lines are for $V_{\rm o} = 300$ km s^-1; " ${\it dashed}$ '' lines correspond to $V_{\rm o} = f(M)$ so that $V_{\rm o} = 340$ km s^-1 at $3~M_{\odot}$ and 420 km s^-1 for $30~M_{\odot}$ .
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$\begin{figure} \par\includegraphics[width=14.5cm,clip]{3051fig5.eps} \end{figure}$	Figure 5: HR diagrams of the studied Be stars. a) Apparent ( $\log L/L_{\odot},\log T_{\rm eff}$ ) with evolutionary tracks without rotation. b) Surface averaged ( $\log L/L_{\odot},\log T_{\rm eff}$ ) and evolutionary tracks with initial an equatorial rotation velocity $V_{\rm o} = 300$ km s^-1 for all masses.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{3051fig6.eps} \end{figure}$	Figure 6: Age ratios $\tau /\tau _{\rm MS}$ of the studied Be stars against the mass. a) Parameters derived using evolutionary tracks without rotation; b) parameters derived using evolutionary tracks with rotation.
Open with DEXTER