All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{nagae-fig1.eps} \end{figure}$ Figure 1: Computational region.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig2.eps} \end{figure}$ Figure 2: Density contours in the orbital plane of the typical RLOF case, but in a semi-detached binary system ( $\gamma =1.01$ , $c_{\rm s}=0.02$ ).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig3.eps} \par\end{figure}$ Figure 3: Streamlines and Mach number counters of the typical RLOF case ( $\gamma =1.01$ , $c_{\rm s}=0.02$ ).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig4.eps} \end{figure}$ Figure 4: Density contours in the orbital plane of the RLOF type flow of model B ( $\gamma =5/3$ , $V_{\rm R}=0.01$ ). The left circle shows the mass losing companion star with a radius of 0.25, and the right black dot indicates the mass accreting object with a radius of 0.015.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig5.eps} \end{figure}$ Figure 5: Streamlines and Mach number contours in the orbital plane of the same model B as in Fig. 2. The Mach number contours are represented by the shade, and the numbers in the figure show typical Mach numbers. Streamlines are generated from points separated by the same distance. We observe that the flow rotates counterclockwise around the companion, which is a typical feature of RLOF type flows.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig6.eps} \end{figure}$ Figure 6: Comparison of two RLOF type flows. Density contours in the orbital plane are shown. Left: model a ( $\gamma =1.01$ , $V_{\rm R}=0.06$ ); right: model D ( $\gamma =5/3$ , $V_{\rm R}=0.12$ ). We observe spiral shocks which are typical to RLOF.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig7.eps} \end{figure}$ Figure 7: Density contours in the orbital plane of the model E ( $\gamma =5/3$ , $V_{\rm R}=0.68$ ). We observe very complicated shock patterns.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig8.eps} \end{figure}$ Figure 8: Streamlines and Mach number contours in the orbital plane of the same model E as in Fig. 7.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig9.eps} \end{figure}$ Figure 9: Density contours and stream lines in the orbital plane of the model b ( $\gamma =1.01$ , $V_{\rm R}=0.46$ ).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig10.eps} \end{figure}$ Figure 10: A schematic diagram of an intermediate flow model E.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig11.eps} \end{figure}$ Figure 11: Density contours in the orbital plane of a typical wind accretion flow model g ( $\gamma =1.01$ , $V_{\rm R}=2.86$ ). We observe a conical bow shock attached to the accreting object, which is a typical feature of the wind accretion flow.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig12.eps} \end{figure}$ Figure 12: Stream lines of the model g as in Fig. 11. Numbers are magnitude of normalized velocity.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig13.eps} \end{figure}$ Figure 13: Density contours of the model g $^{\prime }$ ( $\gamma =1.01$ , $V_{\rm R}=2.85$ ) calculated on the nested grid. Two blow-ups close to the accreting star are shown. Compare the present figure with Fig. 11. We observe that the bow shock is slightly jaggy compared with Fig. 10. This is due to the reduced numerical viscosity.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{nagae-fig14.eps} \end{figure}$ Figure 14: Mass accretion ratio, defined by the ratio of the mass accretion rate to the mass loss rate, as a function of $V_{\rm R}$ . The horizontal axis is $V_{\rm R}$ and the vertical one is the mass accretion ratio. The dash-dotted line is our empirical formula for the mass accretion ratio: $0.18 \times 10^{-0.75V_{\rm R}}$ , while the upper line is the fit valid for large $V_{\rm R}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{nagae-fig15.eps} \end{figure}$ Figure 15: Log-log plot of the Mass accretion ratio as a function of the wind velocity at the position of the Roche lobe. The upper line shows a simple Hoyle-Lyttleton formula as given by Eq. (5). The lower line shows another empirical formula $f = 5.0\times10^{-3}~V_{\rm R}^{-4}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{nagae-fig1.eps} \end{figure}$	Figure 1: Computational region.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig2.eps} \end{figure}$	Figure 2: Density contours in the orbital plane of the typical RLOF case, but in a semi-detached binary system ( $\gamma =1.01$ , $c_{\rm s}=0.02$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig3.eps} \par\end{figure}$	Figure 3: Streamlines and Mach number counters of the typical RLOF case ( $\gamma =1.01$ , $c_{\rm s}=0.02$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig4.eps} \end{figure}$	Figure 4: Density contours in the orbital plane of the RLOF type flow of model B ( $\gamma =5/3$ , $V_{\rm R}=0.01$ ). The left circle shows the mass losing companion star with a radius of 0.25, and the right black dot indicates the mass accreting object with a radius of 0.015.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig6.eps} \end{figure}$	Figure 6: Comparison of two RLOF type flows. Density contours in the orbital plane are shown. Left: model a ( $\gamma =1.01$ , $V_{\rm R}=0.06$ ); right: model D ( $\gamma =5/3$ , $V_{\rm R}=0.12$ ). We observe spiral shocks which are typical to RLOF.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig7.eps} \end{figure}$	Figure 7: Density contours in the orbital plane of the model E ( $\gamma =5/3$ , $V_{\rm R}=0.68$ ). We observe very complicated shock patterns.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig8.eps} \end{figure}$	Figure 8: Streamlines and Mach number contours in the orbital plane of the same model E as in Fig. 7.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig9.eps} \end{figure}$	Figure 9: Density contours and stream lines in the orbital plane of the model b ( $\gamma =1.01$ , $V_{\rm R}=0.46$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig10.eps} \end{figure}$	Figure 10: A schematic diagram of an intermediate flow model E.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig11.eps} \end{figure}$	Figure 11: Density contours in the orbital plane of a typical wind accretion flow model g ( $\gamma =1.01$ , $V_{\rm R}=2.86$ ). We observe a conical bow shock attached to the accreting object, which is a typical feature of the wind accretion flow.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig12.eps} \end{figure}$	Figure 12: Stream lines of the model g as in Fig. 11. Numbers are magnitude of normalized velocity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{nagae-fig13.eps} \end{figure}$	Figure 13: Density contours of the model g $^{\prime }$ ( $\gamma =1.01$ , $V_{\rm R}=2.85$ ) calculated on the nested grid. Two blow-ups close to the accreting star are shown. Compare the present figure with Fig. 11. We observe that the bow shock is slightly jaggy compared with Fig. 10. This is due to the reduced numerical viscosity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{nagae-fig14.eps} \end{figure}$	Figure 14: Mass accretion ratio, defined by the ratio of the mass accretion rate to the mass loss rate, as a function of $V_{\rm R}$ . The horizontal axis is $V_{\rm R}$ and the vertical one is the mass accretion ratio. The dash-dotted line is our empirical formula for the mass accretion ratio: $0.18 \times 10^{-0.75V_{\rm R}}$ , while the upper line is the fit valid for large $V_{\rm R}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{nagae-fig15.eps} \end{figure}$	Figure 15: Log-log plot of the Mass accretion ratio as a function of the wind velocity at the position of the Roche lobe. The upper line shows a simple Hoyle-Lyttleton formula as given by Eq. (5). The lower line shows another empirical formula $f = 5.0\times10^{-3}~V_{\rm R}^{-4}$ .
Open with DEXTER