Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2432fg1a.eps}\par\includegra... ...ip]{2432fg1b.eps}\par\includegraphics[width=8cm,clip]{2432fg1c.eps} \end{figure}$ Figure 1: Plots of the logarithm of density of Run A ( top), Run B ( middle) and Run C ( bottom) after 45 t₀; the coordinates are in units of $R_{\rm g}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f2.eps} \end{figure}$ Figure 2: Time evolution of accretion rate $\dot M = -4~\pi~\rho~v_{r}~H$ in the equatorial plane at $r = 4~R_{\rm g}$ . In Run C the accretion rate is always higher than in the other simulations, perhaps due to the boundary conditions. After 21 t₀, the flare coming from the boundary layer destabilizes the accretion flow and increases its rate in Run B.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa2432f3.eps} \end{figure}$ Figure 3: Poloidal slice at $r = 10~R_{\rm g}$ of the mass accretion/outflow rate $\dot M = -4~\pi~\rho~v_{r}~H$ of Runs A ( top) and B ( bottom) at different times. The emergence of an additional outflow component is visible at about 40 $^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f4.eps} \end{figure}$ Figure 4: Time evolution of the ejection peaks and the accretion disk in Run A ( top) and Run B ( bottom). While the accretion/outflow rates seem to reach an asymptotic value in Run A, they are highly variable in Run B due to the flary conditions inside the BL.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa2432f5.eps} \end{figure}$ Figure 5: Efficiency of the ejection mechanism, calculated as the ratio of the outflow rate in the ejection peak to the accretion rate in the equatorial plane plotted for Runs A ( top) and B ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{aa2432f6.eps} \end{figure}$ Figure 6: Structure of the accretion flow after 14 t₀: density. The density increases in the BL by more than an order of magnitude with respect to the accretion flow, in Run A, the open boundary representing the inner sink arranges for a density decrease by a factor of 4-5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f7.eps} \end{figure}$ Figure 7: Structure of the accretion flow after 14 t₀: ratio of angular momentum to Keplerian angular momentum. In Run B the accretion flow is always rotating super-Keplerian and the angular momentum of the flow in Run A drops below the Keplerian angular momentum for distances smaller than about 3 $R_{\rm g}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f8.eps} \end{figure}$ Figure 8: Structure of the accretion flow after 14 t₀: pressure. The thermal pressure is enhanced in Run B inside the BL by six orders of magnitude with respect to Run A.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f9.eps} \end{figure}$ Figure 9: Structure of the accretion flow after 14 t₀: azimuthal magnetic field component. The emergence of the boundary layer also creates a peak in the magnetic field at its surface, which is perhaps caused by compression in strong shocks inside it.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2432f10a.eps}\par\includeg... ...{2432f10b.eps}\par\includegraphics[width=8.2cm,clip]{2432f10c.eps} \end{figure}$ Figure 10: Plots of the total poloidal current $r~B_{\phi}$ after 45 t₀ for Run A ( top), Run B ( middle) and Run C ( bottom) with logarithmic contour lines from I = 0 to I = 10¹² A.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{aa2432f11.eps} \end{figure}$ Figure 11: Structure of the ejection component at $\theta = 45^{\circ }$ after 45 t₀: density. Knots with enhanced density are present.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{aa2432f12.eps} \end{figure}$ Figure 12: Structure of the ejection component at $\theta = 45^{\circ }$ after 45 t₀: temperature.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2432fg1a.eps}\par\includegra... ...ip]{2432fg1b.eps}\par\includegraphics[width=8cm,clip]{2432fg1c.eps} \end{figure}$	Figure 1: Plots of the logarithm of density of Run A ( top), Run B ( middle) and Run C ( bottom) after 45 t₀; the coordinates are in units of $R_{\rm g}$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f2.eps} \end{figure}$	Figure 2: Time evolution of accretion rate $\dot M = -4~\pi~\rho~v_{r}~H$ in the equatorial plane at $r = 4~R_{\rm g}$ . In Run C the accretion rate is always higher than in the other simulations, perhaps due to the boundary conditions. After 21 t₀, the flare coming from the boundary layer destabilizes the accretion flow and increases its rate in Run B.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa2432f3.eps} \end{figure}$	Figure 3: Poloidal slice at $r = 10~R_{\rm g}$ of the mass accretion/outflow rate $\dot M = -4~\pi~\rho~v_{r}~H$ of Runs A ( top) and B ( bottom) at different times. The emergence of an additional outflow component is visible at about 40 $^{\circ }$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f4.eps} \end{figure}$	Figure 4: Time evolution of the ejection peaks and the accretion disk in Run A ( top) and Run B ( bottom). While the accretion/outflow rates seem to reach an asymptotic value in Run A, they are highly variable in Run B due to the flary conditions inside the BL.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa2432f5.eps} \end{figure}$	Figure 5: Efficiency of the ejection mechanism, calculated as the ratio of the outflow rate in the ejection peak to the accretion rate in the equatorial plane plotted for Runs A ( top) and B ( bottom).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{aa2432f6.eps} \end{figure}$	Figure 6: Structure of the accretion flow after 14 t₀: density. The density increases in the BL by more than an order of magnitude with respect to the accretion flow, in Run A, the open boundary representing the inner sink arranges for a density decrease by a factor of 4-5.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f7.eps} \end{figure}$	Figure 7: Structure of the accretion flow after 14 t₀: ratio of angular momentum to Keplerian angular momentum. In Run B the accretion flow is always rotating super-Keplerian and the angular momentum of the flow in Run A drops below the Keplerian angular momentum for distances smaller than about 3 $R_{\rm g}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f8.eps} \end{figure}$	Figure 8: Structure of the accretion flow after 14 t₀: pressure. The thermal pressure is enhanced in Run B inside the BL by six orders of magnitude with respect to Run A.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{aa2432f9.eps} \end{figure}$	Figure 9: Structure of the accretion flow after 14 t₀: azimuthal magnetic field component. The emergence of the boundary layer also creates a peak in the magnetic field at its surface, which is perhaps caused by compression in strong shocks inside it.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2432f10a.eps}\par\includeg... ...{2432f10b.eps}\par\includegraphics[width=8.2cm,clip]{2432f10c.eps} \end{figure}$	Figure 10: Plots of the total poloidal current $r~B_{\phi}$ after 45 t₀ for Run A ( top), Run B ( middle) and Run C ( bottom) with logarithmic contour lines from I = 0 to I = 10¹² A.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{aa2432f11.eps} \end{figure}$	Figure 11: Structure of the ejection component at $\theta = 45^{\circ }$ after 45 t₀: density. Knots with enhanced density are present.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{aa2432f12.eps} \end{figure}$	Figure 12: Structure of the ejection component at $\theta = 45^{\circ }$ after 45 t₀: temperature.
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