All Figures

$\begin{figure} \includegraphics[width=12cm,clip]{7703fig1.ps} \end{figure}$ Figure 1: 2D color maps of electron temperature for four characteristic accretion sates A, B, C, and D. The length scale for the horizontal axies is logarithmic in units of $R_{\rm in}$ , so that the size of a box is 20 $R_{\rm S}$ . The temperature is given in logarithmic scale in K.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{7703fig2.ps} \end{figure}$ Figure 2: 2D color maps of the emission at four frequencies: $\log \nu=11$ , 12, 14, and 18 Hz ( from left to the right) and for four distinct accretion sates A, B, C, and D ( from top to bottom; see the main text for more detail on states A, B, C, and D). The length scale for the horizontal axies is logarithmic in units of $R_{\rm in}$ , so that the size of a box is 20 $R_{\rm S}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig3.ps}\end{figure}$ Figure 3: Radiation spectra corresponding to accretion states A, B, C, and D, respectively (only thermal electrons were included). The mass accretion rate at the outer boundary of the simulation is $\dot{M}_{\rm B}= 3.7 \times 10^{-6}~{M_{\odot}/\rm yr}$ and central black hole mass is $M_{\rm BH}=3.7 \times 10^{6}~{M_{\odot}}$ . In state A, the mass accretion rate (through the inner boundary of the flow) in units of $\dot{M}_{\rm B}$ equals about 0.11; in the state B is $\sim$ 0.009; in the state C; when torus does not accrete, it decreases to 0.001. For state D $\dot{M}_{\rm a}$ increases to 0.048.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig4.ps} \end{figure}$ Figure 4: Synchrotron spectra emitted at accretion state D in the radio band, seen by observers at the different locations.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig5.ps} \end{figure}$ Figure 5: Upper panel: time evolution of 31 spectra in time intervals from 2.33 to 2.4. Time is given in Keplerian orbital time (see PB03); ${t_{\rm Keplerian}=2 \pi R_{\rm B}/ \sqrt {GM/R_{\rm B}}} = 10^7$ s, where ${R_{\rm B}=10^3 R_{\rm g}}$ . Each curve represents a monochromatic flux at different frequencies: 10¹¹ (solid), 10¹² (long dash), 10¹⁴ (short dash), and 10¹⁸ Hz (dotted line). X-ray (10¹⁸ Hz) variability is very low in comparison to the variability at the other wavelengths. Observations at 10¹¹-10¹⁴ Hz can be used to distinguish the characteristic accretion states B and D. Lower panel: the time dependence of the mass accretion rate for comparison.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig6.ps} \end{figure}$ Figure 6: Spectra emitted at accretion states B, C, and D. The model was calculated for the parameters of Sgr A*. Spectra for thermal electrons are marked by B, C, D, and hybrid electron distribution including non-thermal electrons is marked by "nt B'', "nt C'', and "nt D''. The parameters for non-thermal electrons are: $\eta =0.1\%$ , p=2.5, $\gamma _{\rm max}=10^{5}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig7.ps} \end{figure}$ Figure 7: As in Fig. 6 for different parameters of non-thermal electron distribution. Note the change in the non-thermal spectra. The parameters for non-thermal electrons are: $\eta =0.1\%$ , p=2.5, $\gamma _{\rm max}=10^{6}$ . The observational data are taken from: Narayan et al. (1998), Genzel et al. (2003), Ghez et al. (2004), Baganoff et al. (2003), Porquet et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig8.ps} \end{figure}$ Figure 8: Faraday rotation RM for four accretion states. The x axis shows the angle of the observer, and the y axis shows the RM values as a function of inclination as predicted by the models. Different lines show modeled RM for different simulation time (A, B, C, D). A state is marked as a solid line, B as a long dash line, C as a short dash line, and D as a dotted line, Two straight lines show the lower and upper limits from Marrone et al. (2006).
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In the text

$\begin{figure} \includegraphics[width=12cm,clip]{7703fig1.ps} \end{figure}$	Figure 1: 2D color maps of electron temperature for four characteristic accretion sates A, B, C, and D. The length scale for the horizontal axies is logarithmic in units of $R_{\rm in}$ , so that the size of a box is 20 $R_{\rm S}$ . The temperature is given in logarithmic scale in K.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{7703fig2.ps} \end{figure}$	Figure 2: 2D color maps of the emission at four frequencies: $\log \nu=11$ , 12, 14, and 18 Hz ( from left to the right) and for four distinct accretion sates A, B, C, and D ( from top to bottom; see the main text for more detail on states A, B, C, and D). The length scale for the horizontal axies is logarithmic in units of $R_{\rm in}$ , so that the size of a box is 20 $R_{\rm S}$ .
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig4.ps} \end{figure}$	Figure 4: Synchrotron spectra emitted at accretion state D in the radio band, seen by observers at the different locations.
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig6.ps} \end{figure}$	Figure 6: Spectra emitted at accretion states B, C, and D. The model was calculated for the parameters of Sgr A*. Spectra for thermal electrons are marked by B, C, D, and hybrid electron distribution including non-thermal electrons is marked by "nt B'', "nt C'', and "nt D''. The parameters for non-thermal electrons are: $\eta =0.1\%$ , p=2.5, $\gamma _{\rm max}=10^{5}$ .
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{7703fig7.ps} \end{figure}$	Figure 7: As in Fig. 6 for different parameters of non-thermal electron distribution. Note the change in the non-thermal spectra. The parameters for non-thermal electrons are: $\eta =0.1\%$ , p=2.5, $\gamma _{\rm max}=10^{6}$ . The observational data are taken from: Narayan et al. (1998), Genzel et al. (2003), Ghez et al. (2004), Baganoff et al. (2003), Porquet et al. (2003).
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