Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{0223fig1.eps} \end{figure}$ Figure 1: Visible setup of the AK Sco disk system using the estimated inclination of $63^\circ$ . The disk shape is modeled according to pressure scale height, gray scale coding is logarithmic surface density in ${\rm g}/{\rm cm}^2$ . The disk extent is 12 AU.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0223fig2.eps} \end{figure}$ Figure 2: Linear surface density ( ${\rm g}/{\rm cm}^2$ ) of the inner circumbinary disk of the DQ Tau system after 50 orbital periods. Scaling is in AU. The spiral structure in the circumbinary disk induced by the binary is clearly seen.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0223fig3.eps} \end{figure}$ Figure 3: The spiral arms onto the circumstellar environment for the DQ Tau system after 50 orbital periods. The gray scale follows logarithmic surface density annotated with iso-lines. Plotted is the region inside the circumbinary disk gap which is located at 0.4 AU. The binary is in apastron phase.
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm,clip]{0223fig4.eps}\hspace*{2mm} \includegraphics[width=4.4cm,clip]{0223fig5.eps} \end{figure}$ Figure 4: Circumstellar disks logarithmic density structure for Dual-Grid simulation ( left) and SPH simulation ( right) while approaching periastron. The binary separation is about 0.1 AU.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0223fig6.eps} \end{figure}$ Figure 5: Contribution of the different heating/cooling terms to the rate of temperature change (DQ Tau after 50 orbital periods). Only the inner part of the system is displayed. The irradiation irr and the radiative cooling -cool match exactly beyond 0.4 AU.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223fig7.eps} \end{figure}$ Figure 6: Contribution of the different heating/cooling terms to the rate of temperature change (DQ Tau after 50 orbital periods). Plotted is the outer circumbinary disk part of the system. The irradiation by the central stars and the radiative cooling match exactly (topmost dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223fig8.eps} \end{figure}$ Figure 7: Computed SED of DQ Tau. Crosses show observational data taken from Mathieu et al. (1997).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223fig9.eps} \end{figure}$ Figure 8: Azimuthally averaged surface temperature of the equilibrium DQ Tau circumbinary disk.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223figA.eps} \end{figure}$ Figure 9: Computed SED of AK Sco with parameters and observational data (crosses with error-bars) taken from Alencar et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0223figB.eps} \end{figure}$ Figure 10: Computed SED of the AK Sco system with best-fit parameters. Crosses with error-bars show observational data taken from Alencar et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223figC.eps} \end{figure}$ Figure 11: Azimuthally averaged surface temperature of the equilibrium AK Sco circumbinary disk.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0223figD.eps} \end{figure}$ Figure 12: Profiles of the circumstellar material along the connecting line of the binary at apastron in the system of DQ Tau (stellar radii $0.008~{\rm AU}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0223figE.eps} \end{figure}$ Figure 13: Circumstellar material in the DQ Tau system after 41 orbital periods, corresponding to Fig. 12. Gray scale coding is velocity magnitude annotated with vector glyphs, isolines are equally spaced logarithmic surface density. The stellar cores are the white circles.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0223fig1.eps} \end{figure}$	Figure 1: Visible setup of the AK Sco disk system using the estimated inclination of $63^\circ$ . The disk shape is modeled according to pressure scale height, gray scale coding is logarithmic surface density in ${\rm g}/{\rm cm}^2$ . The disk extent is 12 AU.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0223fig2.eps} \end{figure}$	Figure 2: Linear surface density ( ${\rm g}/{\rm cm}^2$ ) of the inner circumbinary disk of the DQ Tau system after 50 orbital periods. Scaling is in AU. The spiral structure in the circumbinary disk induced by the binary is clearly seen.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0223fig3.eps} \end{figure}$	Figure 3: The spiral arms onto the circumstellar environment for the DQ Tau system after 50 orbital periods. The gray scale follows logarithmic surface density annotated with iso-lines. Plotted is the region inside the circumbinary disk gap which is located at 0.4 AU. The binary is in apastron phase.
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$\begin{figure} \par\includegraphics[width=4.4cm,clip]{0223fig4.eps}\hspace*{2mm} \includegraphics[width=4.4cm,clip]{0223fig5.eps} \end{figure}$	Figure 4: Circumstellar disks logarithmic density structure for Dual-Grid simulation ( left) and SPH simulation ( right) while approaching periastron. The binary separation is about 0.1 AU.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0223fig6.eps} \end{figure}$	Figure 5: Contribution of the different heating/cooling terms to the rate of temperature change (DQ Tau after 50 orbital periods). Only the inner part of the system is displayed. The irradiation irr and the radiative cooling -cool match exactly beyond 0.4 AU.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223fig7.eps} \end{figure}$	Figure 6: Contribution of the different heating/cooling terms to the rate of temperature change (DQ Tau after 50 orbital periods). Plotted is the outer circumbinary disk part of the system. The irradiation by the central stars and the radiative cooling match exactly (topmost dashed line).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223fig8.eps} \end{figure}$	Figure 7: Computed SED of DQ Tau. Crosses show observational data taken from Mathieu et al. (1997).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223fig9.eps} \end{figure}$	Figure 8: Azimuthally averaged surface temperature of the equilibrium DQ Tau circumbinary disk.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223figA.eps} \end{figure}$	Figure 9: Computed SED of AK Sco with parameters and observational data (crosses with error-bars) taken from Alencar et al. (2003).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0223figB.eps} \end{figure}$	Figure 10: Computed SED of the AK Sco system with best-fit parameters. Crosses with error-bars show observational data taken from Alencar et al. (2003).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0223figC.eps} \end{figure}$	Figure 11: Azimuthally averaged surface temperature of the equilibrium AK Sco circumbinary disk.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0223figD.eps} \end{figure}$	Figure 12: Profiles of the circumstellar material along the connecting line of the binary at apastron in the system of DQ Tau (stellar radii $0.008~{\rm AU}$ ).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0223figE.eps} \end{figure}$	Figure 13: Circumstellar material in the DQ Tau system after 41 orbital periods, corresponding to Fig. 12. Gray scale coding is velocity magnitude annotated with vector glyphs, isolines are equally spaced logarithmic surface density. The stellar cores are the white circles.
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