All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{KerrPaWi1.ps} \end{figure}$ Figure 1: The black hole event horizon $r_{\rm H}$ , the innermost stable circular orbit $r_{\rm ISCO}$ , and $\beta$ as defined in Eq. (2), as functions of the black hole spin parameter a. Both $r_{\rm H}$ and $r_{\rm ISCO}$ are given in units of $GM_{\rm BH}/c^2 = 0.5R_{{\rm s}}$ .
Open with DEXTER

In the text

$\begin{figure} \begin{tabular}{cc} \psfig{file=IIr00d.ps,width=4.2cm} & \psfig... ....ps,width=4.2cm} & \psfig{file=IIr00y.ps,width=4.2cm}\end{tabular} \end{figure}$ Figure 2: Initial configuration at the start of the simulations for model r00-64. The density is displayed in the orbital plane ( left) and in two orthogonal planes perpendicular to the equator ( right). It is given in g cm^-3with contours spaced logarithmically in steps of 0.5 dex. The arrows in the density plots indicate the velocity field. The temperature and electron fraction ( $Y_{\rm e}$ ) are displayed in the orbital plane. The temperature is measured in MeV, its contours are labelled with the corresponding values. The contours of electron fraction are spaced linearly in steps of 0.02.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=Ir00d2.ps,width=4.2cm} & \psfig{... ....ps,width=4.2cm} & \psfig{file=Ir00y2.ps,width=4.2cm}\end{tabular} \end{figure}$ Figure 3: Density distribution for models r00-64 in the orbital plane ( left) and perpendicular to it ( right) at about 11 ms after the start of the simulations. It is given in g cm^-3with contours spaced logarithmically in steps of 0.5 dex. The arrows in the density plots indicate the velocity field. The temperature and electron fraction ( $Y_{\rm e}$ ) are displayed in the orbital plane. The temperature is measured in MeV, its contours are labelled with the corresponding values. The contours of electron fraction are spaced linearly in steps of 0.02.
Open with DEXTER

In the text

$\begin{figure} \begin{tabular}{cc} \psfig{file=gasmas1bb.ps,width=4.2cm} & \\ [... ...width=4.2cm} & \psfig{file=BHaccr1bb.ps,width=4.2cm}\end{tabular} \end{figure}$ Figure 4: Mass accretion rate of the black hole and and gas mass on the grid as functions of time for models r00-64, al3-64 and al4-64 with increasing disk viscosity. Gas mass on the grid as functions of time for the reference model r00-64, the low-mass torus model ir1-64, and the high-mass torus models ir4-64, ir5-64, ri4-64, and ar2-64.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=Ial3d2.ps,width=4.2cm} & \psfig{... ...width=4.2cm} & \psfig{file=Ial4t2.ps,width=4.2cm}\\ \end{tabular} \end{figure}$ Figure 5: Density and temperature distribution for models al3-64 ( left) and al4-64 ( right) with disk viscosities of $\alpha = 0.01$ and $\alpha = 0.1$ , respectively. The density is given in g cm^-3with contours spaced logarithmically in steps of 0.5 dex. The arrows in the density plots indicate the velocity field. The temperature is measured in MeV, its contours are labelled with the corresponding values.
Open with DEXTER

In the text

$\begin{figure}\par\mbox{\includegraphics[width=4.4cm]{maxrho64aa.ps} ~~ \includegraphics[width=4.4cm]{maxtem64aa.ps} } \par\end{figure}$ Figure 6: Maximum values of gas density ( left) and temperature ( right) on the grid as functions of time for models r00-64, al3-64 and al4-64 with increasing disk viscosity.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=IIro2d2.ps,width=4.2cm} & \psfig... ...s,width=4.2cm} & \psfig{file=ar1t.ps,width=4.2cm}\\ \end{tabular} \end{figure}$ Figure 7: Density and temperature distribution for models ro2-64 ( left) and ar1-64 ( right) for a corotating black hole, with disk viscosities of $\alpha = 0.0$ , and $\alpha = 0.1$ , respectively. The density is given in g cm^-3with contours spaced logarithmically in steps of 0.5 dex. The arrows in the density plots indicate the velocity field. The temperature is measured in MeV, its contours are labelled with the corresponding values.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=vphiss2.ps,width=4.0cm} & \psfig... ...th=4.0cm} & \psfig{file=R9CI_vrad.ps,width=4.0cm}\\ \end{tabular} \end{figure}$ Figure 8: Left panels: the dots represent the azimuthal velocities $v_\varphi (d)$ (normalised to the speed of light) of all zones in the equatorial plane of the reference model r00-64, and the high disk-viscosity model ar1-64 with corotating black hole, at the times after the start of the simulation indicated in the plots. The thin solid line gives the average value of the azimuthal velocities and the bold solid line the local Keplerian velocity $v_{\rm Kepler}(d)$ of the Artemova et al. (1996) potential as a function of the equatorial radius d (Eq. (3)). The inner vacuum boundary of the computational grid, is located at the arithmetic mean of the event horizon and innermost stable circular orbit (ISCO) of the central black hole. Right panels: the dots give the radial velocities v_r(d) (normalised to the speed of light) as a function of the equatorial radius d for all grid zones in the equatorial plane of the reference model r00-64 and the high disk-viscosity model al4-64, at the same times. The solid lines represent the mean values of all zones within binning intervals of 3 km.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=IIir4d3.ps,width=4.2cm} & \psfig... ...s,width=4.2cm} & \psfig{file=ar2t.ps,width=4.2cm}\\ \end{tabular} \end{figure}$ Figure 9: Density and temperature distribution for high-mass torus models with nonrotating black hole and without disk viscosity (ir4-64; left) and with corotating black hole and disk viscosity $\alpha = 0.1$ (ar2-64; right) at about 20 ms after the start of the simulations. The arrows indicate the velocity field. The density is given in g cm^-3 with contours spaced logarithmically in steps of 0.5 dex. The temperature is measured in MeV, its contours are labelled with the corresponding values.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.4cm,clip]{neuIIdw2p.ps} ~~ \includegraphics[width=4.4cm,clip]{ensIIdw2p.ps} } \par\end{figure}$ Figure 10: Total neutrino luminosities ( left) and cumulative energy radiated in neutrinos ( right) as functions of time for the reference model r00-64, the low-mass torus model ir1-64, and the high-mass torus models ir4-64, ir5-64, ri4-64, and ar2-64.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=IIro2y2.ps,width=4.2cm} & \psfig... ...s,width=4.2cm} & \psfig{file=ar2y.ps,width=4.2cm}\\ \end{tabular} \end{figure}$ Figure 11: Electron fraction in the orbital plane for models ro2-64, ar1-64, ir4-64 and ar2-64, in the orbital plane at about 11 ms after the start of the simulations. The contours are spaced linearly in steps of 0.02.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=e_nu_r00.ps,width=4.2cm} & \psfi... ...dth=4.2cm} & \psfig{file=total_nu_r00.ps,width=4.2cm}\end{tabular} \end{figure}$ Figure 12: Neutrino energy loss rates per unit area in the orbital plane for model r00-64 at 20 ms after the start of the simulations. The plotted values show the logarithm of the rates in erg cm^-2 s^-1, obtained by integration of the local energy loss rates per unit of volume from z = 0 to infinity. The top left panel gives the results for electron neutrinos, the top right panel for electron antineutrinos, the lower left panel for the sum of muon and tau neutrinos and antineutrinos, and the lower right panel the total values for neutrinos and antineutrinos of all flavors. The contours are spaced in steps of 0.5 dex, bold lines are labelled with their corresponding values. The grey shading emphasises the emission levels, dark grey representing the largest energy loss by neutrino emission.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=acceffIIdw2p.ps,width=4.2cm} & \... ...dth=4.2cm} & \psfig{file=anni02IIdw2p.ps,width=4.2cm}\end{tabular} \end{figure}$ Figure 13: Conversion efficiency of rest-mass energy to neutrinos, $q_{\nu}\equiv L_{\nu}/(\dot Mc^2)$ ( top left), conversion efficiency of neutrino energy to electron-positron pairs by neutrino-antineutrino annihilation, $q_{\nu\bar\nu} \equiv \dot E_{\nu\bar\nu}/L_{\nu}$ ( top right), integral rate of energy deposition by neutrino-antineutrino annihilation around the accretion torus, $\dot{E}_{\nu\bar{\nu}}$ ( bottom left), and cumulative energy deposition by $\nu\bar\nu$ annihilation, $E_{\nu\bar{\nu}}$ ( bottom right), as functions of time for the same set of models shown in Figs. 4, and 10.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=anni01bb.ps,width=4.2cm} & \psfig{file=anni03bb.ps,width=4.2cm}\\ \end{tabular} \end{figure}$ Figure 14: Integral rate of energy deposition by neutrino-antineutrino annihilation around the accretion torus, $\dot{E}_{\nu\bar{\nu}}$ ( left) and conversion efficiency of neutrino energy to electron-positron pairs by neutrino-antineutrino annihilation $q_{\nu\bar\nu} \equiv \dot E_{\nu\bar\nu}/L_{\nu}$ ( right), as functions of time for selected 64-resolution models with the same torus mass but different torus viscosity. The models are the same as in Figs. 4 and 6.
Open with DEXTER

In the text

$\begin{figure}\begin{tabular}{cc} \psfig{file=r00annmap.ps,width=4.2cm} & \psf... ...th=4.2cm} & \psfig{file=ar2annmap.ps,width=4.2cm}\\ \end{tabular} \end{figure}$ Figure 15: Maps of the local energy deposition rates (in erg cm^-3 s^-1) by $\nu\bar\nu$ annihilation to $\rm e^+e^-$ pairs in the surroundings of the accretion torus for models r00-64, ro2-64, ro5-64, and ar2-64 at a time 20 ms after the start of the simulation. The solid contour lines in a plane perpendicular to the equatorial plane represent values averaged over azimuthal angles around the z-axis. The contours are logarithmically spaced in steps of 0.5 dex and the grey shading emphasises the levels with dark grey meaning high energy deposition rate. The energy deposition rate was evaluated only in that region around the torus where the baryon mass density is below $10^{11}~{\rm g~cm}^{-3}$ . The white octagonal area around the centre with a semidiameter of one Schwarzschild radius indicates the presence of the central black hole. The dotted contour lines represent levels of constant values of the azimuthally averaged mass density, also logarithmically spaced with intervals of 0.5 dex; the bold dotted line corresponds to $\rho=10^{10}~{\rm g~cm}^{-3}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{KerrPaWi1.ps} \end{figure}$	Figure 1: The black hole event horizon $r_{\rm H}$ , the innermost stable circular orbit $r_{\rm ISCO}$ , and $\beta$ as defined in Eq. (2), as functions of the black hole spin parameter a. Both $r_{\rm H}$ and $r_{\rm ISCO}$ are given in units of $GM_{\rm BH}/c^2 = 0.5R_{{\rm s}}$ .
Open with DEXTER

$\begin{figure} \begin{tabular}{cc} \psfig{file=gasmas1bb.ps,width=4.2cm} & \\ [... ...width=4.2cm} & \psfig{file=BHaccr1bb.ps,width=4.2cm}\end{tabular} \end{figure}$	Figure 4: Mass accretion rate of the black hole and and gas mass on the grid as functions of time for models r00-64, al3-64 and al4-64 with increasing disk viscosity. Gas mass on the grid as functions of time for the reference model r00-64, the low-mass torus model ir1-64, and the high-mass torus models ir4-64, ir5-64, ri4-64, and ar2-64.
Open with DEXTER

$\begin{figure}\par\mbox{\includegraphics[width=4.4cm]{maxrho64aa.ps} ~~ \includegraphics[width=4.4cm]{maxtem64aa.ps} } \par\end{figure}$	Figure 6: Maximum values of gas density ( left) and temperature ( right) on the grid as functions of time for models r00-64, al3-64 and al4-64 with increasing disk viscosity.
Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=4.4cm,clip]{neuIIdw2p.ps} ~~ \includegraphics[width=4.4cm,clip]{ensIIdw2p.ps} } \par\end{figure}$	Figure 10: Total neutrino luminosities ( left) and cumulative energy radiated in neutrinos ( right) as functions of time for the reference model r00-64, the low-mass torus model ir1-64, and the high-mass torus models ir4-64, ir5-64, ri4-64, and ar2-64.
Open with DEXTER

$\begin{figure}\begin{tabular}{cc} \psfig{file=IIro2y2.ps,width=4.2cm} & \psfig... ...s,width=4.2cm} & \psfig{file=ar2y.ps,width=4.2cm}\\ \end{tabular} \end{figure}$	Figure 11: Electron fraction in the orbital plane for models ro2-64, ar1-64, ir4-64 and ar2-64, in the orbital plane at about 11 ms after the start of the simulations. The contours are spaced linearly in steps of 0.02.
Open with DEXTER