All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f1.ps}\end{figure}$ Figure 1: Parameter space for viewing accreting X-ray pulsars. The region below the solid line corresponds to visibility of two polar caps with gravitational light bending neglected. The region below the dashed line corresponds to visibility of two caps with the gravitational light deflection $\Delta _{\rm g}=30^\circ$ . The shaded region is the part of the parameter space in which pulses would be detectable if radiation is strongly beamed. The horizontal dotted line corresponds to the angle between the rotation and magnetic axes $\beta =50^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f2.ps}\end{figure}$ Figure 2: The probability of classifying a pulsar as single peaked as a function of the threshold below which the second peak is not detectable.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f3.ps}\end{figure}$ Figure 3: Left panel: the probability of seeing only one polar cap as a function of the maximal gravitational light deflection. The non-relativistic case corresponds to $\Delta _{\rm g}=0$ . Right panel; the probability of seeing only one cap as a function of the beaming angle $\alpha$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f4.ps}\par\end{figure}$ Figure 4: The probability of seeing only one polar cap as a function of the maximal gravitational light deflection when the beam is described by the from F₂. The non-relativistic case corresponds to $\Delta _{\rm g}=0$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f5.ps}\par\end{figure}$ Figure 5: The probability of observing the data in models pencil beam parameterized by the the maximum angle between the magnetic and rotation axis $\beta _{\rm {max}}$ . The solid line corresponds to the data set ${\cal S}_1$ , and the short-dashed line corresponds to the data set ${\cal S}_2$ . The long-dashed line corresponds to the data set ${\cal S}_3$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f6.ps}\par\end{figure}$ Figure 6: The probability of observing the data in fan beam models parameterized by the the maximum angle between the magnetic and rotation axis $\beta _{\rm {max}}$ : thin lines - fan beam F₁, thick lines - fan beam F₂. The solid line corresponds to the data set ${\cal S}_1$ , and the short-dashed line corresponds to the data set ${\cal S}_2$ . The long-dashed line corresponds to the data set ${\cal S}_3$ .
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In the text

$\begin{figure} \par\includegraphics[width=5.1cm,clip]{3320-f7a.ps}\hspace*{0.4cm... ...b.ps}\hspace*{0.4cm} \includegraphics[width=5.1cm,clip]{3320-f7c.ps}\end{figure}$ Figure 7: Each panel presents the region containing the models that are consistent with the data at the level of 60%, 90%, and 99%. The three panels correspond to the three datasets.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3320-f8.ps}\end{figure}$ Figure 8: The value of the gravitational light bending as a function of the emission angle, measured from the radial direction for photons emitted at different initial radii. The maximum gravitational light deflection is the value of deflection for the initial angle of $90^\circ$ , i.e. parallel to the surface.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3320-f9.ps}\end{figure}$ Figure 9: The ratio of the stellar radius to the gravitational radius as a function of mass for several neutron star equations of state. The labels are BPAL12 - Prakash et al. (1997), SBD - Sahu et al. (1993), BB1 and BB2 - Baldo et al. (1997), while SS1 and SS2 correspond to the MIT Bag model of strange quark matter (Witten 1984) with two different densities at zero pressure.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f2.ps}\end{figure}$	Figure 2: The probability of classifying a pulsar as single peaked as a function of the threshold below which the second peak is not detectable.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f3.ps}\end{figure}$	Figure 3: Left panel: the probability of seeing only one polar cap as a function of the maximal gravitational light deflection. The non-relativistic case corresponds to $\Delta _{\rm g}=0$ . Right panel; the probability of seeing only one cap as a function of the beaming angle $\alpha$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f4.ps}\par\end{figure}$	Figure 4: The probability of seeing only one polar cap as a function of the maximal gravitational light deflection when the beam is described by the from F₂. The non-relativistic case corresponds to $\Delta _{\rm g}=0$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3320-f5.ps}\par\end{figure}$	Figure 5: The probability of observing the data in models pencil beam parameterized by the the maximum angle between the magnetic and rotation axis $\beta _{\rm {max}}$ . The solid line corresponds to the data set ${\cal S}_1$ , and the short-dashed line corresponds to the data set ${\cal S}_2$ . The long-dashed line corresponds to the data set ${\cal S}_3$ .
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$\begin{figure} \par\includegraphics[width=5.1cm,clip]{3320-f7a.ps}\hspace{0.4cm... ...b.ps}\hspace{0.4cm} \includegraphics[width=5.1cm,clip]{3320-f7c.ps}\end{figure}$	Figure 7: Each panel presents the region containing the models that are consistent with the data at the level of 60%, 90%, and 99%. The three panels correspond to the three datasets.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3320-f8.ps}\end{figure}$	Figure 8: The value of the gravitational light bending as a function of the emission angle, measured from the radial direction for photons emitted at different initial radii. The maximum gravitational light deflection is the value of deflection for the initial angle of $90^\circ$ , i.e. parallel to the surface.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3320-f9.ps}\end{figure}$	Figure 9: The ratio of the stellar radius to the gravitational radius as a function of mass for several neutron star equations of state. The labels are BPAL12 - Prakash et al. (1997), SBD - Sahu et al. (1993), BB1 and BB2 - Baldo et al. (1997), while SS1 and SS2 correspond to the MIT Bag model of strange quark matter (Witten 1984) with two different densities at zero pressure.
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