All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0741fig1a.eps}\hspace*{4mm} \includegraphics[width=8.8cm,clip]{0741fig1b.eps} \end{figure}$ Figure 1: Illustration of the spot distribution created by flares that illuminate the underlying disk. The plane of the disk is shown, as viewed from the top, along the symmetry axis; (x,y) coordinates are scaled with the black hole gravitational radius, $R_{\rm {}g}$ . Left: a snapshot of an instantaneous spot distribution. Right: effective covering of the disk surface by radiating belts in a time-integrated observation. Different realizations of the spot distribution have been explored in the paper (see Table 2).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0741fig2a.eps}\hspace*{5mm} \includegraphics[width=7cm,clip]{0741fig2b.eps} \end{figure}$ Figure 2: Local reflection spectrum of an individual hot spot, which arises due to irradiation of the disk surface by a flare. Left: broad energy range is shown (log-log scale) with the intrinsic spectral resolution $E/\delta {E}=30$ . The dotted line shows the incident spectrum. Right: an expanded part of the same spectrum around the iron line energy (linear scale). Here, a higher intrinsic spectral resolution was adopted, $E/\delta {E}=100$ . In both panels, common parameters are $M=10^8 ~M_{\odot}$ , $\dot{m}=0.001$ , $R=18 ~R_{\rm g}$ , $F_{\rm {}X}=10^{15}$ erg s^-1 cm^-2, $\Gamma =1.9$ (see Sect. 3.1 for details).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0741fig3.eps} \end{figure}$ Figure 3: The reflection spectrum from the spotted disk. The local intrinsic emissivity decreases ( $\beta _{\rm {}rad}=3$ ) as radius increases up to $R_{\rm{}out}=50 ~R_{\rm{}g}$ . The case of a Schwarzschild black hole, a=0, and moderate inclination, $i=30{\hbox {$^\circ $ }}$ (panel a)), can be compared with the case a=0, $i=60{\hbox {$^\circ $ }}$ (panel b)), rapidly rotating case a=0.998, $i=30{\hbox {$^\circ $ }}$ (panel c)), and a=0.998, $i=60{\hbox {$^\circ $ }}$ . Dotted lines show the case of a relativistically smeared monochromatic line at 6.4 keV superimposed on a flat continuum.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0741fig4.eps} \end{figure}$ Figure 4: The dependence of the luminosity of the uniformly radiating disk belts on the inclination angle for the maximally rotating Kerr black hole a=0.998. Power law spectrum and no radial dependence of the intensity were assumed.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0741fig5.eps} \end{figure}$ Figure 5: The dependence of the luminosity of uniformly radiating disk on the inclination angle with isotropic local emission, limb brightening ( $I(\mu )\propto 5-4\mu$ ), and limb darkening ( $I(\mu )\propto 1+2.06\mu$ ). The radial emissivity law $\propto$ r^-3 was assumed together with a power-law spectral shape.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0741fig6.eps} \end{figure}$ Figure 6: Two random realizations of the same spot distribution (thin lines) and the original local emission (thick line histogram) for model A; the ratio of the two random realizations are shown below. The local input spectrum is the sum of the primary (flare) emission and the reflected (spot) component, without any limb-darkening.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0741fig7.eps} \end{figure}$ Figure 7: Fractional variability amplitude calculated as a function of energy. The model A ( $i=30^{\circ }$ ; upper panel), the model D ( $i=30^{\circ }$ ; middle panel), and the model D at high observed inclination ( $i=70^{\circ }$ ; bottom panel). Duration of a single observation 10⁵ s, number of exposures 300.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0741fig8.eps} \end{figure}$ Figure 8: The dependence of the normalized dispersion measured at 1 keV on the inclination angle of observation for model A (upper panel, continuous line), model J (upper panel, dashed line) and model L (lower panel, middle curve). Two other curves in the lower panel show the result of increasing the mean number of flares to 3000 and decreasing the mean number of flares to 300. Number of exposures was 100.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0741fig4.eps} \end{figure}$	Figure 4: The dependence of the luminosity of the uniformly radiating disk belts on the inclination angle for the maximally rotating Kerr black hole a=0.998. Power law spectrum and no radial dependence of the intensity were assumed.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0741fig5.eps} \end{figure}$	Figure 5: The dependence of the luminosity of uniformly radiating disk on the inclination angle with isotropic local emission, limb brightening ( $I(\mu )\propto 5-4\mu$ ), and limb darkening ( $I(\mu )\propto 1+2.06\mu$ ). The radial emissivity law $\propto$ r^-3 was assumed together with a power-law spectral shape.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0741fig6.eps} \end{figure}$	Figure 6: Two random realizations of the same spot distribution (thin lines) and the original local emission (thick line histogram) for model A; the ratio of the two random realizations are shown below. The local input spectrum is the sum of the primary (flare) emission and the reflected (spot) component, without any limb-darkening.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0741fig7.eps} \end{figure}$	Figure 7: Fractional variability amplitude calculated as a function of energy. The model A ( $i=30^{\circ }$ ; upper panel), the model D ( $i=30^{\circ }$ ; middle panel), and the model D at high observed inclination ( $i=70^{\circ }$ ; bottom panel). Duration of a single observation 10⁵ s, number of exposures 300.
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