All Figures

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1441f1.eps}\end{figure}$ Figure 1: The pressure p against the energy density $\rho$ for the EOSs used in the paper: APR (dashed line), GNH3 (dotted line), and BPAL12 (solid line). The empty circles correspond to the central density of a non-rotating stellar model with a gravitational mass equal to $1.35~M_{\odot}$ (Table 1).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1441f2.eps}\end{figure}$ Figure 2: Gravitational mass of static isolated stars against area radius for the APR (dashed line), GNH3 (dotted line) and BPAL12 (solid line) EOSs.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1441f3.eps}\end{figure}$ Figure 3: The adiabatic index $\gamma$ against the energy density $\rho$ for the EOSs used in our computations: APR (dashed line), GNH3 (dotted line), and BPAL12 (solid line). The empty circles correspond to the central density of a non-rotating stellar model with a gravitational mass equal to $1.35~M_{\odot}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.15cm,clip]{1441f4a.eps}\hs... ...ace*{2mm} \includegraphics[angle=-90,width=8.15cm,clip]{1441f4f.eps}\end{figure}$ Figure 4: Baryon number density isocontours in the coordinate plane y=0 (containing the rotation axis) ( left panels) and in the coordinate plane z=0 (orbital plane) ( right panels), for configurations close to the mass-shedding limit. The upper (resp. middle, lower) panels correspond to the GNH3 (resp. APR, BPAL12) EOS. The thick solid lines denote stellar surfaces.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.65cm,clip]{1441f5.eps}\end{figure}$ Figure 5: Orbital binding energy $E_{\rm bind} = M_{\rm ADM} - M_\infty$ of the binary system versus frequency of gravitational waves (twice the orbital frequency) along three irrotational quasi-equilibrium sequences. The lines (dotted - GNH3, dashed - APR, solid - BPAL12) were plotted using the fit described in the text, whereas the points represent actual data. Thin solid line touching the bottom-right corner shows the 3rd post-Newtonian approximation for point masses derived by Blanchet (2002). The lower thin dotted curve corresponds to the Newtonian limit for point masses.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.45cm,clip]{1441f6.eps}\end{figure}$ Figure 6: Orbital binding energy of the binary system minus the (point mass) Newtonian term $-k_{\rm N} f^{2/3}$ versus frequency of gravitational waves (twice the orbital frequency) along three irrotational quasi-equilibrium sequences. Thin solid line shows the 3rd post-Newtonian approximation for point masses by Blanchet (2002). Slightly below there is the 2PN line (thin, dashed) and the 1PN one (thin, long dash-dotted). For the comparison post-Newtonian approximation by Damour et al. (2000) - 3PN (dashed-dotted thin line) and 2PN (thin, long dashed) are also plotted.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1441f7.eps}\end{figure}$ Figure 7: Difference $E_{\rm bind} - E_{\rm bind}^{\rm 3PN}$ between the binding energy of irrotational binary neutron stars built upon a realistic equation of state and the binding energy of binary point masses in the 3PN approximation of Blanchet (2002). The dots correspond to numerical results and the lines to polynomial fits to them (see text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.05cm,clip]{1441f8.eps}\end{figure}$ Figure 8: Energy spectrum of GW waves emitted by the binary neutron star system versus frequency of gravitational waves (twice the orbital frequency) along three irrotational quasi-equilibrium sequences. The straight lines correspond to the Newtonian dependence of energy multiplied by 1, 0.8, 0.75 and 0.6.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{1441f9.eps}\end{figure}$ Figure 9: Gravitational mass versus stellar radius for sequences of static neutron stars described by the Akmal et al. (1998) EOS (solid line) and polytropic EOS with $\gamma =2$ (dotted line) and $\gamma =2.5$ (dashed line). Configurations with gravitational mass $1.35~M_{\odot}$ (marked by a circle) described by polytropic EOSs have the same compaction parameter, M/R = 0.176, as a neutron star configuration based on the APR EOS.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.65cm,clip]{1441f10.eps}\end{figure}$ Figure 10: Binding energy of a binary neutron star system as a function of gravitational wave frequency for the APR EOS (thick solid line) and two corresponding polytropic EOS with $\gamma =2.5$ (dashed line) and $\gamma =2$ (dotted line). Static isolated NSs have M/R=0.176 and $M=1.35~{M}_\odot$ . The thin solid line shows the 3PN approximation for point masses by Blanchet (2002), Eq. (8).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1441f1.eps}\end{figure}$	Figure 1: The pressure p against the energy density $\rho$ for the EOSs used in the paper: APR (dashed line), GNH3 (dotted line), and BPAL12 (solid line). The empty circles correspond to the central density of a non-rotating stellar model with a gravitational mass equal to $1.35~M_{\odot}$ (Table 1).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1441f2.eps}\end{figure}$	Figure 2: Gravitational mass of static isolated stars against area radius for the APR (dashed line), GNH3 (dotted line) and BPAL12 (solid line) EOSs.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1441f3.eps}\end{figure}$	Figure 3: The adiabatic index $\gamma$ against the energy density $\rho$ for the EOSs used in our computations: APR (dashed line), GNH3 (dotted line), and BPAL12 (solid line). The empty circles correspond to the central density of a non-rotating stellar model with a gravitational mass equal to $1.35~M_{\odot}$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8.15cm,clip]{1441f4a.eps}\hs... ...ace*{2mm} \includegraphics[angle=-90,width=8.15cm,clip]{1441f4f.eps}\end{figure}$	Figure 4: Baryon number density isocontours in the coordinate plane y=0 (containing the rotation axis) ( left panels) and in the coordinate plane z=0 (orbital plane) ( right panels), for configurations close to the mass-shedding limit. The upper (resp. middle, lower) panels correspond to the GNH3 (resp. APR, BPAL12) EOS. The thick solid lines denote stellar surfaces.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1441f7.eps}\end{figure}$	Figure 7: Difference $E_{\rm bind} - E_{\rm bind}^{\rm 3PN}$ between the binding energy of irrotational binary neutron stars built upon a realistic equation of state and the binding energy of binary point masses in the 3PN approximation of Blanchet (2002). The dots correspond to numerical results and the lines to polynomial fits to them (see text for details).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.05cm,clip]{1441f8.eps}\end{figure}$	Figure 8: Energy spectrum of GW waves emitted by the binary neutron star system versus frequency of gravitational waves (twice the orbital frequency) along three irrotational quasi-equilibrium sequences. The straight lines correspond to the Newtonian dependence of energy multiplied by 1, 0.8, 0.75 and 0.6.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.65cm,clip]{1441f10.eps}\end{figure}$	Figure 10: Binding energy of a binary neutron star system as a function of gravitational wave frequency for the APR EOS (thick solid line) and two corresponding polytropic EOS with $\gamma =2.5$ (dashed line) and $\gamma =2$ (dotted line). Static isolated NSs have M/R=0.176 and $M=1.35~{M}_\odot$ . The thin solid line shows the 3PN approximation for point masses by Blanchet (2002), Eq. (8).
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