Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{5.8cm}{!}{\includegraphics[clip]{0227fig1.eps}}\end{figure}$ Figure 1: A schematic diagram of the surface flow of a companion star in a semi-detached binary system: H, L1 and L2 denote eddies associated with a high/low pressure, respectively. Typical velocity vectors are shown with numbers.
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In the text

$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics[clip]{0227fig2.eps}}\end{figure}$ Figure 2: Equidensity surface ( $\log \protect\rho=-2$ ) of the companion star and the streamlines starting from the equidensity surface of $\log \protect\rho=-2.5$ ; A mass ratio of q=0.33 and a specific heat ratio of $\protect\gamma=5/3$ , are adopted. The top panel is viewed from the north, while the bottom panel is viewed from the opposite side of the L1-point. H-, L1-, and L2-eddies can be seen.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{0227fig3.eps}}\end{figure}$ Figure 3: Equidensity surface ( $\log \protect\rho=-3.1$ ) of the accretion disc is shown; q=0.33 and $\protect\gamma=1.01$ are adopted in this figure. The size of the whole computed region is $2.0 \times 1.0 \times 0.5$ (including companion star), and the number of grid points is $201 \times 101 \times 51$ . Note, however, that the region to the right of the L1 point is shown to exhibit only the accretion disc. We may observe a pair of spiral shocks and a shock associated with the L1 stream.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{0227fig4.eps}}\end{figure}$ Figure 4: Same as in Fig. 2 but for a mass ratio of q=2.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0227fig5.eps}\end{figure}$ Figure 5: Same as in Fig. 3 but here the equidensity surface of $\log \protect\rho=-4.5$ is shown for a mass ratio of q=2.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0227fig6.eps}\end{figure}$ Figure 6: Surface flow on the companion star in a binary with q=0.05; equidensity surface ( $\log \protect\rho=-2.5$ ) of the companion star and the streamlines starting from the equidensity surface of $\log \protect\rho=-3$ . Note that a small fraction of the gas flows through the L2 point as well as the L1 point because of the shallow gravitational potential.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{0227fig7.eps}}\end{figure}$ Figure 7: Doppler map constructed from the horizontal components of velocity, V_x and V_y, at the equidensity surface of $\log \protect\rho=-2.5$ for the companion star (denoted by the cross) and $\log \protect\rho=-3.9$ for the accretion disc (denoted by the plus). In this figure q=1. Note that the following figures are placed upside down in order to compare our results with those of other authors. The critical Roche surface and the ballistic orbit of the L1 stream are also shown for purpose of reference. The upper and the lower dot show the centre of mass of the companion and that of the primary, while the middle dot (at the L1 point) denotes the common centre of gravity.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{0227fig8.eps}}\end{figure}$ Figure 8: The surface of the companion is divided into four quadrants as shown in the right bottom sub-panel. We can examine the contribution from each surface region. The number in each Doppler map corresponds to the quadrant in the sub-panel. Note that the same data is used as in Fig. 7.
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In the text

$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics[clip]{0227fig9.eps}}\end{figure}$ Figure 9: Constructed Doppler map as a model of RX J0019.8+2156 with q=3: in order to have a velocity scale, we assume $A\Omega _{\rm orb}=330$ km s^-1. The observed intensity of the He II ${\protect\lambda}4686$ emission byDeufel et al. (1999) has a peak around $V_{x}\sim 100$ km s^-1 and $V_{y}\sim 100$ km s^-1 (with our velocity sign), denoted here by a dotted circle.
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In the text

$\begin{figure} \par\resizebox{5.8cm}{!}{\includegraphics[clip]{0227fig1.eps}}\end{figure}$	Figure 1: A schematic diagram of the surface flow of a companion star in a semi-detached binary system: H, L1 and L2 denote eddies associated with a high/low pressure, respectively. Typical velocity vectors are shown with numbers.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{0227fig4.eps}}\end{figure}$	Figure 4: Same as in Fig. 2 but for a mass ratio of q=2.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0227fig5.eps}\end{figure}$	Figure 5: Same as in Fig. 3 but here the equidensity surface of $\log \protect\rho=-4.5$ is shown for a mass ratio of q=2.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0227fig6.eps}\end{figure}$	Figure 6: Surface flow on the companion star in a binary with q=0.05; equidensity surface ( $\log \protect\rho=-2.5$ ) of the companion star and the streamlines starting from the equidensity surface of $\log \protect\rho=-3$ . Note that a small fraction of the gas flows through the L2 point as well as the L1 point because of the shallow gravitational potential.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{0227fig8.eps}}\end{figure}$	Figure 8: The surface of the companion is divided into four quadrants as shown in the right bottom sub-panel. We can examine the contribution from each surface region. The number in each Doppler map corresponds to the quadrant in the sub-panel. Note that the same data is used as in Fig. 7.
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$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics[clip]{0227fig9.eps}}\end{figure}$	Figure 9: Constructed Doppler map as a model of RX J0019.8+2156 with q=3: in order to have a velocity scale, we assume $A\Omega _{\rm orb}=330$ km s^-1. The observed intensity of the He II ${\protect\lambda}4686$ emission byDeufel et al. (1999) has a peak around $V_{x}\sim 100$ km s^-1 and $V_{y}\sim 100$ km s^-1 (with our velocity sign), denoted here by a dotted circle.
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