\documentstyle{l-aa}
\begin{document}
%==============================================================================
\def\Msun{M_\odot}
\def\Teff{T_{eff}}
\def\Lsun{L_\odot}
\def\Rsun{R_\odot}
\def\Mdot{\dot M}
\def\ue{ue}
\def\Mstar{M*}
\def\Lstar{L*}

\setcounter{table}{1}
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
     1&2&3&4&5&6&7&8&9&10&11 \\ \hline
      & & & & & & & & &   \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
C6\_m & $3 \cdot 10^{-7}$ & 2.0035 & ~7.78 & 11.39 & 0.99 & 1.11 & ~0.0870 & 0.0693 & 0.0232 & 0.0169 \\
C6\_n &                   & ------ & ----- & ----- & ---- & ---- & ------- & ------ & ------ & ------ \\
      & & & & & & & & & \\[-3mm]
C5\_m & $5 \cdot 10^{-7}$ & 2.0277 & ~7.87 & 13.00 & 1.14 & 0.80 & ~0.1502 & 0.1197 & 0.0401 & 0.0321 \\
C5\_n &                   & 2.0512 & ~7.97 & ~9.02 & 0.79 & 0.97 & ~0.1947 & 0.1551 & 0.0519 & 0.0223 \\
      & & & & & & & & & \\[-3mm]
C4\_m & $1 \cdot 10^{-6}$ & 2.1052 & ~8.18 & 14.60 & 1.30 & 0.53 & ~0.3126 & 0.2491 & 0.0832 & 0.0721 \\
C4\_n &                   & 2.1272 & ~8.26 & 11.39 & 1.02 & 0.61 & ~0.3744 & 0.2984 & 0.0995 & 0.0563 \\
      & & & & & & & & & \\[-3mm]
C3\_m & $3 \cdot 10^{-6}$ & 2.3394 & ~9.09 & 15.86 & 1.49 & 0.29 & ~0.9642 & 0.7685 & 0.2507 & 0.2349 \\
C3\_n &                   & 2.3736 & ~9.22 & 12.91 & 1.22 & 0.33 & ~1.1050 & 0.8808 & 0.2857 & 0.1912 \\
      & & & & & & & & & \\[-3mm]
C2\_m & $1 \cdot 10^{-5}$ & 2.8814 & 11.19 & 15.07 & 1.57 & 0.15 & ~3.1430 & 2.5050 & 0.7431 & 0.7440 \\
C2\_n &                   & 2.9417 & 11.42 & 11.97 & 1.26 & 0.17 & ~3.5980 & 2.8670 & 0.8353 & 0.5909 \\
      & & & & & & & & & \\[-3mm]
C1\_m & $3 \cdot 10^{-5}$ & 3.6333 & 14.11 & 12.72 & 1.49 & 0.07 & ~9.2440 & 7.3670 & 1.7750 & 1.8840 \\
C1\_n &                   & 3.7549 & 14.58 & ~9.32 & 1.11 & 0.10 & 11.1600 & 8.8940 & 2.0450 & 1.3811 \\ 
                  \hline \hline
\end{tabular} 
\caption[]
{
Main properties of the circumstellar gas/dust shell around an {\em Oxygen
star\/} with $\Mstar=1 \, \Msun, \Lstar=1 \cdot 10^4 \, \Lsun, \Teff=3000$~K as
a function of adopted mass loss rate $\Mdot$ (column 2).  Columns 3 to 11 list the
following quantities:  (3):  dust condensation radius $r_1$ in [10$^{14}$ cm],
(4):  $r_1$ in stellar radii $r_\ast$, (5):  the terminal gas velocity \ue\ in
[km/s], (6): \ue\ in units of the local escape velocity $v_{\rm esc}(r_1)$,
(7):  the terminal drift velocity $w - u$ in units of
\ue, (8):  the total optical depth of the dust shell in the visual ($\lambda\,
0.55 \, \mu$m), (9): $\tau_{10}$, the optical depth at $\lambda\, 10 \, \mu$m, 
(10): $\tau_{\rm F}$, the flux-averaged optical depth (cf.~Eq.\ref{tauF}), 
and (11):
the ratio of momentum flux in the outflow to the photon momentum flux, $\beta =
\Mdot \ue\ c / \Lstar$.  Dust consists of {\em astronomical silicates\/} with
properties given in Table1.  The initial velocity (gas and dust) at the
inner boundary $r_1$ is taken to be $u_1 = 2$~km/s.  For each mass loss rate,
the second row (model designations Ci\_n) lists the corresponding results from a
model calculation ignoring gas pressure, (---) indicating that no steady state
solution was found.  The velocity structure and resulting spectral energy
distribution for models C6\_m, C3\_m and C1\_m (including gas pressure) are
displayed in Fig.2.
}
\label{tab2}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
D5\_m & $3 \cdot 10^{-6}$ & ~4.3621 & ~5.26 & 17.96 & 1.15 & 0.55 & ~0.3740 & ~0.2981 & 0.0761 & 0.0532 \\
D5\_n &                   & ~4.4096 & ~5.32 & 15.10 & 0.97 & 0.61 & ~0.4381 & ~0.3492 & 0.0893 & 0.0447 \\
      & & & & & & & & & \\[-3mm]
D4\_m & $1 \cdot 10^{-5}$ & ~4.9238 & ~5.94 & 20.51 & 1.40 & 0.29 & ~1.2260 & ~0.9774 & 0.2521 & 0.2026 \\
D4\_n &                   & ~4.9957 & ~6.03 & 18.04 & 1.24 & 0.31 & ~1.3600 & ~1.0840 & 0.2793 & 0.1782 \\
      & & & & & & & & & \\[-3mm]
D3\_m & $3 \cdot 10^{-5}$ & ~6.0076 & ~7.25 & 20.12 & 1.51 & 0.16 & ~3.4940 & ~2.7850 & 0.6922 & 0.5961 \\
D3\_n &                   & ~6.1165 & ~7.38 & 17.51 & 1.33 & 0.18 & ~3.8460 & ~3.0650 & 0.7554 & 0.5189 \\
      & & & & & & & & & \\[-3mm]
D2\_m & $1 \cdot 10^{-4}$ & ~7.8759 & ~9.50 & 16.96 & 1.46 & 0.08 & 11.2100 & ~8.9380 & 1.8730 & 1.6753 \\
D2\_n &                   & ~8.0928 & ~9.76 & 14.06 & 1.23 & 0.10 & 12.7100 & 10.1300 & 2.0660 & 1.3881 \\
      & & & & & & & & & \\[-3mm]
D1\_m & $3 \cdot 10^{-4}$ & 10.378~ & 12.52 & 13.71 & 1.36 & 0.03 & 32.3300 & 25.7700 & 4.3940 & 4.0605 \\
D1\_n &                   & 10.945~ & 13.20 & 10.71 & 1.09 & 0.06 & 38.6300 & 30.7900 & 5.0890 & 3.1735 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab2} but for an Oxygen star with $\Mstar=4 \, \Msun, \Lstar=5
\cdot 10^4 \, \Lsun, \Teff=2500$~K.  The velocity structure and resulting
spectral energy distribution for models D5\_m, D3\_m and D1\_m are displayed in
Fig.3.
}
\label{tab3}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
E5\_m & $1 \cdot 10^{-5}$ & 12.009 & ~5.12 & 34.79 & 2.34 & 0.61 & ~0.2184 & ~0.1740 & 0.0442 & 0.0429 \\
E5\_n &                   & 12.023 & ~5.13 & 33.63 & 2.26 & 0.62 & ~0.2248 & ~0.1791 & 0.0455 & 0.0415 \\
      & & & & & & & & & \\[-3mm]
E4\_m & $3 \cdot 10^{-5}$ & 12.966 & ~5.53 & 38.31 & 2.68 & 0.34 & ~0.6936 & ~0.5528 & 0.1421 & 0.1419 \\
E4\_n &                   & 12.990 & ~5.54 & 37.19 & 2.60 & 0.35 & ~0.7099 & ~0.5657 & 0.1455 & 0.1378 \\
      & & & & & & & & & \\[-3mm]
E3\_m & $1 \cdot 10^{-4}$ & 15.549 & ~6.63 & 38.17 & 2.92 & 0.19 & ~2.2620 & ~1.8030 & 0.4593 & 0.4712 \\
E3\_n &                   & 15.567 & ~6.64 & 36.93 & 2.83 & 0.19 & ~2.3080 & ~1.8390 & 0.4684 & 0.4558 \\
      & & & & & & & & & \\[-3mm]
E2\_m & $3 \cdot 10^{-4}$ & 19.720 & ~8.41 & 33.98 & 2.93 & 0.11 & ~6.4970 & ~5.1780 & 1.1920 & 1.2583 \\
E2\_n &                   & 19.720 & ~8.41 & 32.56 & 2.81 & 0.11 & ~6.6270 & ~5.2810 & 1.2140 & 1.2057 \\
      & & & & & & & & & \\[-3mm]
E1\_m & $1 \cdot 10^{-3}$ & 26.339 & 11.23 & 27.29 & 2.72 & 0.05 & 21.0000 & 16.7400 & 3.0640 & 3.3700 \\
E1\_n &                   & 26.412 & 11.26 & 25.71 & 2.56 & 0.06 & 21.5600 & 17.1800 & 3.1320 & 3.1728 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab2} but for an Oxygen star with $\Mstar=10 \, \Msun,
\Lstar=4 \cdot 10^5 \, \Lsun, \Teff=2500$~K, and $u_1 = 4$~km/s.  The velocity
structure and resulting spectral energy distribution for models E5\_m, E3\_m and
E1\_m are displayed in Fig.4.
}
\label{tab4}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
F4\_m & $1 \cdot 10^{-5}$ & 12.109 & 5.16 & 26.19 & 1.02 & 0.71 & 0.2719 & 0.2167 & 0.0552 & 0.0323 \\
F4\_n &                   & 12.140 & 5.18 & 24.33 & 0.95 & 0.73 & 0.2893 & 0.2305 & 0.0587 & 0.0300 \\
      & & & & & & & & & \\[-3mm]
F3\_m & $3 \cdot 10^{-5}$ & 13.140 & 5.60 & 31.83 & 1.29 & 0.37 & 0.8002 & 0.6378 & 0.1643 & 0.1179 \\
F3\_n &                   & 13.189 & 5.62 & 30.33 & 1.23 & 0.39 & 0.8328 & 0.6637 & 0.1710 & 0.1124 \\
      & & & & & & & & & \\[-3mm]
F2\_m & $1 \cdot 10^{-4}$ & 15.849 & 6.76 & 32.85 & 1.47 & 0.20 & 2.5290 & 2.0160 & 0.5113 & 0.4055 \\
F2\_n &                   & 15.911 & 6.78 & 31.25 & 1.40 & 0.21 & 2.6180 & 2.0860 & 0.5285 & 0.3858 \\
      & & & & & & & & & \\[-3mm]
F1\_m & $3 \cdot 10^{-4}$ & 20.077 & 8.56 & 29.15 & 1.46 & 0.11 & 7.3010 & 5.8190 & 1.3150 & 1.0796 \\
F1\_n &                   & 20.137 & 8.59 & 27.26 & 1.37 & 0.12 & 7.5830 & 6.0430 & 1.3580 & 1.0097 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab2} but for an Oxygen star with $\Mstar=30 \, \Msun,
\Lstar=4 \cdot 10^5 \, \Lsun, \Teff=2500$~K, and $u_1 = 4$~km/s.  The velocity
structure and resulting spectral energy distribution for models F4\_m, F2\_m and
F1\_m are displayed in Fig.5.
}
\label{tab5}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
G6\_m & $3 \cdot 10^{-7}$ & 3.356  & 5.79 & 11.15 &  1.25 & 2.21 & ~0.1630 & 0.0008 & 0.0154 & 0.0165 \\
G6\_n &                   & 3.357  & 5.79 & ~3.01 &  0.34 & 4.25 & ~0.2908 & 0.0015 & 0.0273 & 0.0045 \\
      & & & & & & & & & \\[-3mm]
G5\_m & $5 \cdot 10^{-7}$ & 3.364  & 5.81 & 12.49 &  1.41 & 1.61 & ~0.3017 & 0.0016 & 0.0283 & 0.0308 \\
G5\_n &                   & 3.363  & 5.80 & ~7.54 &  0.85 & 2.06 & ~0.4044 & 0.0021 & 0.0376 & 0.0186 \\
      & & & & & & & & & \\[-3mm]
G4\_m & $1 \cdot 10^{-6}$ & 3.378  & 5.83 & 14.07 &  1.59 & 1.04 & ~0.6922 & 0.0036 & 0.0631 & 0.0694 \\
G4\_n &                   & 3.381  & 5.84 & 10.11 &  1.14 & 1.22 & ~0.8540 & 0.0044 & 0.0769 & 0.0499 \\
      & & & & & & & & & \\[-3mm]
G3\_m & $3 \cdot 10^{-6}$ & 3.467  & 5.98 & 15.35 &  1.75 & 0.51 & ~2.5320 & 0.0131 & 0.2044 & 0.2274 \\
G3\_n &                   & 3.478  & 6.00 & 11.83 &  1.35 & 0.57 & ~2.9840 & 0.0154 & 0.2344 & 0.1753 \\
      & & & & & & & & & \\[-3mm]
G2\_m & $1 \cdot 10^{-5}$ & 3.695  & 6.38 & 13.90 &  1.64 & 0.21 & 10.6000 & 0.0548 & 0.6051 & 0.6862 \\
G2\_n &                   & 3.714  & 6.41 & 10.02 &  1.19 & 0.24 & 12.5500 & 0.0649 & 0.6734 & 0.4951 \\
      & & & & & & & & & \\[-3mm]
G1\_m & $3 \cdot 10^{-5}$ & 4.105  & 7.09 & 10.43 &  1.30 & 0.07 & 39.8500 & 0.2061 & 1.3170 & 1.5456 \\
G1\_n &                   & 4.169  & 7.20 & ~5.71 &  0.72 & 0.12 & 51.9200 & 0.2685 & 1.5020 & 0.8455 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab2} but for a {\em Carbon star\/} with $\Mstar=1 \, \Msun,
\Lstar=1 \cdot 10^4 \, \Lsun$, and $\Teff=2000$~K.  Dust consists of {\em
graphite\/} with properties given in Tab.~\ref{tab1}.  The velocity structure
and resulting spectral energy distribution for models G6\_m, G3\_m and G1\_m are
displayed in Fig.6.
}
\label{tab6}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
H6\_m & $3 \cdot 10^{-6}$ &  7.546 & 5.82 & 19.83 &  1.93 & 1.14 &~~0.6350 & 0.0033 & 0.0581 & 0.0587 \\
H6\_n &                   &  7.553 & 5.83 & 17.10 &  1.67 & 1.22 &~~0.7144 & 0.0037 & 0.0650 & 0.0507 \\
      & & & & & & & & & \\[-3mm]
H5\_m & $1 \cdot 10^{-5}$ &  7.764 & 5.99 & 22.00 &  2.17 & 0.52 &~~2.6260 & 0.0136 & 0.2110 & 0.2172 \\
H5\_n &                   &  7.786 & 6.01 & 19.52 &  1.93 & 0.54 &~~2.8820 & 0.0149 & 0.2281 & 0.1928 \\
      & & & & & & & & & \\[-3mm]
H4\_m & $3 \cdot 10^{-5}$ &  8.236 & 6.36 & 20.03 &  2.04 & 0.23 &~~9.6690 & 0.0500 & 0.5706 & 0.5936 \\
H4\_n &                   &  8.266 & 6.38 & 17.28 &  1.76 & 0.25 &~10.6000 & 0.0548 & 0.6062 & 0.5118 \\
      & & & & & & & & & \\[-3mm]
H3\_m & $1 \cdot 10^{-4}$ &  9.283 & 7.17 & 14.46 &  1.56 & 0.08 &~42.0000 & 0.2172 & 1.3610 & 1.4284 \\
H3\_n &                   &  9.345 & 7.21 & 11.10 &  1.20 & 0.11 &~47.6100 & 0.2462 & 1.4490 & 1.0960 \\
      & & & & & & & & & \\[-3mm]
H2\_m & $3 \cdot 10^{-4}$ & 10.792 & 8.33 & ~9.68 &  1.13 & 0.02 &155.8000 & 0.8057 & 2.7420 & 2.8676 \\
H2\_n &                   & 10.990 & 8.48 & ~5.52 &  0.65 & 0.06 &200.8000 & 1.0390 & 3.1300 & 1.6349 \\
      & & & & & & & & & \\[-3mm]
H1\_m & $6 \cdot 10^{-4}$ & 12.221 & 9.43 & ~7.69 &  0.95 & 0.01 &333.6000 & 1.7250 & 4.3270 & 4.5594 \\
H1\_n &                   & 12.685 & 9.79 & ~2.20 &  0.28 & 0.06 &501.8000 & 2.5950 & 5.5080 & 1.3026 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab6} but for a Carbon star with $\Mstar=3 \, \Msun, \Lstar=5
\cdot 10^4 \, \Lsun$, and $\Teff=2000$~K.  The velocity structure and resulting
spectral energy distribution for models H6\_m, H4\_m and H2\_m are displayed in
Fig.7.
}
\label{tab7}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
I5\_m & $3 \cdot 10^{-6}$ & ~7.560 & 5.84 & 17.47 &  1.32 & 1.20 &~~0.6955 & 0.0036 & 0.0634 & 0.0518 \\
I5\_n &                   & ~7.561 & 5.84 & 13.91 &  1.05 & 1.34 &~~0.8327 & 0.0043 & 0.0751 & 0.0412 \\
      & & & & & & & & & \\[-3mm]
I4\_m & $1 \cdot 10^{-5}$ & ~7.780 & 6.01 & 20.07 &  1.54 & 0.54 &~~2.8050 & 0.0145 & 0.2230 & 0.1981 \\
I4\_n &                   & ~7.804 & 6.02 & 17.16 &  1.32 & 0.57 &~~3.1610 & 0.0163 & 0.2462 & 0.1694 \\
      & & & & & & & & & \\[-3mm]
I3\_m & $3 \cdot 10^{-5}$ & ~8.266 & 6.38 & 18.02 &  1.42 & 0.24 &~10.3600 & 0.0536 & 0.5968 & 0.5339 \\
I3\_n &                   & ~8.302 & 6.41 & 14.75 &  1.17 & 0.26 &~11.6900 & 0.0604 & 0.6451 & 0.4368 \\
      & & & & & & & & & \\[-3mm]
I2\_m & $8 \cdot 10^{-5}$ & ~9.129 & 7.05 & 13.19 &  1.09 & 0.10 &~35.1400 & 0.1817 & 1.2320 & 1.0427 \\
I2\_n &                   & ~9.196 & 7.10 &  8.96 &  0.75 & 0.14 &~41.8800 & 0.2166 & 1.3470 & 0.7075 \\
      & & & & & & & & & \\[-3mm]
I1\_m & $2 \cdot 10^{-4}$ & 10.278 & 7.93 &  8.17 &  0.72 & 0.03 &114.6000 & 0.5924 & 2.2940 & 1.6127 \\
I1\_n &                   & ------ & ---- &  ---- &  ---- & ---- &-------- & ------ & ------ & ------ \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab6} but for a Carbon star with $\Mstar=5 \, \Msun, \Lstar=5
\cdot 10^4 \, \Lsun$, and $\Teff=2000$~K.  The velocity structure and resulting
spectral energy distribution for models I5\_m, I3\_m and I1\_m are displayed in
Fig.8.
}
\label{tab8}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
J6\_m & $3 \cdot 10^{-7}$ & 2.723 & 4.70 & 10.85 &  1.10 & 1.76 & ~0.1090 & 0.0024 & 0.0175 & 0.0161 \\
J6\_n &                   & ----- & ---- & ----- &  ---- & ---- & ------- & ------ & ------ & ------ \\
      & & & & & & & & & \\[-3mm]
J5\_m & $5 \cdot 10^{-7}$ & 2.730 & 4.71 & 12.30 &  1.25 & 1.27 & ~0.1966 & 0.0043 & 0.0313 & 0.0304 \\
J5\_n &                   & 2.730 & 4.71 & ~6.92 &  0.70 & 1.70 & ~0.2775 & 0.0061 & 0.0439 & 0.0171 \\
      & & & & & & & & & \\[-3mm]
J4\_m & $1 \cdot 10^{-6}$ & 2.744 & 4.74 & 13.96 &  1.42 & 0.83 & ~0.4377 & 0.0096 & 0.0684 & 0.0689 \\
J4\_n &                   & 2.747 & 4.74 & ~9.88 &  1.00 & 0.98 & ~0.5476 & 0.0120 & 0.0848 & 0.0488 \\
      & & & & & & & & & \\[-3mm]
J3\_m & $3 \cdot 10^{-6}$ & 2.827 & 4.88 & 15.41 &  1.59 & 0.42 & ~1.5220 & 0.0332 & 0.2195 & 0.2282 \\
J3\_n &                   & 2.840 & 4.90 & 11.83 &  1.22 & 0.47 & ~1.7940 & 0.0392 & 0.2538 & 0.1752 \\
      & & & & & & & & & \\[-3mm]
J2\_m & $1 \cdot 10^{-5}$ & 3.072 & 5.30 & 14.36 &  1.54 & 0.18 & ~5.8870 & 0.1285 & 0.6639 & 0.7091 \\
J2\_n &                   & 3.098 & 5.35 & 10.46 &  1.13 & 0.21 & ~6.9060 & 0.1508 & 0.7436 & 0.5168 \\
      & & & & & & & & & \\[-3mm]
J1\_m & $3 \cdot 10^{-5}$ & 3.542 & 6.11 & 11.25 &  1.30 & 0.07 & 20.0400 & 0.4374 & 1.5040 & 1.6662 \\
J1\_n &                   & 3.610 & 6.23 & ~6.75 &  0.79 & 0.11 & 25.2300 & 0.5507 & 1.7270 & 0.9993 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab6}, but for dust consisting of {\em amorphous carbon\/}
with properties given in Tab.~\ref{tab1}.  The velocity structure and resulting
spectral energy distribution for models J6\_m, J3\_m and J1\_m are displayed in
Fig.9.
}
\label{tab9}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
K6\_m & $3 \cdot 10^{-6}$  & ~6.126 & 4.73 & 20.09 & 1.76 & 0.90 &~~0.3969 & 0.0087 & 0.0622 & 0.0595 \\
K6\_n &                    & ~6.135 & 4.74 & 17.40 & 1.53 & 0.96 &~~0.4466 & 0.0097 & 0.0698 & 0.0515 \\
      & & & & & & & & & \\[-3mm]
K5\_m & $1 \cdot 10^{-5}$  & ~6.334 & 4.89 & 22.42 & 2.00 & 0.42 &~~1.5580 & 0.0340 & 0.2243 & 0.2214 \\
K5\_n &                    & ~6.356 & 4.91 & 19.97 & 1.78 & 0.45 &~~1.7030 & 0.0372 & 0.2427 & 0.1972 \\
      & & & & & & & & & \\[-3mm]
K4\_m & $3 \cdot 10^{-5}$  & ~6.838 & 5.28 & 20.97 & 1.94 & 0.20 &~~5.3470 & 0.1167 & 0.6198 & 0.6212 \\
K4\_n &                    & ~6.875 & 5.31 & 18.25 & 1.70 & 0.22 &~~5.8140 & 0.1269 & 0.6588 & 0.5407 \\
      & & & & & & & & & \\[-3mm]
K3\_m & $1 \cdot 10^{-4}$  & ~8.039 & 6.21 & 15.94 & 1.60 & 0.08 &~20.7700 & 0.4535 & 1.5450 & 1.5742 \\
K3\_n &                    & ~8.123 & 6.27 & 12.72 & 1.28 & 0.10 &~23.1200 & 0.5047 & 1.6480 & 1.2566 \\
      & & & & & & & & & \\[-3mm]
K2\_m & $3 \cdot 10^{-4}$  & ~9.968 & 7.69 & 11.61 & 1.30 & 0.02 &~67.5200 & 1.4740 & 3.2770 & 3.4403 \\
K2\_n &                    & 10.257 & 7.92 & ~8.04 & 0.91 & 0.05 &~80.3600 & 1.7540 & 3.6570 & 2.3820 \\
      & & & & & & & & & \\[-3mm]
K1\_m & $6 \cdot 10^{-4}$  & 11.784 & 9.10 & ~9.72 & 1.18 & 0.01 &133.0000 & 2.9040 & 5.2360 & 5.7570 \\
K1\_n &                    & 12.357 & 9.54 & ~5.81 & 0.72 & 0.04 &167.3000 & 3.6530 & 6.0970 & 3.4421 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab9} but for a Carbon star with $\Mstar=3 \, \Msun, \Lstar=5
\cdot 10^4 \, \Lsun$, and $\Teff=2000$~K.  The velocity structure and resulting
spectral energy distribution for models K6\_m, K4\_m and K2\_m are displayed in
Fig.10.
}
\label{tab10}
\end{center}
\end{table*}
%==============================================================================
%==============================================================================
\begin{table*}[htb]
\begin{center}
\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|} \hline
      & & & & & & & & & &  \\[-3mm]
Model & $\Mdot$ [$\Msun$/yr] & $r_1$ [$10^{14}$ cm] & $r_1/r_\ast$ 
      & \ue\ [km/s] & $\ue/v_{\rm esc}(r_1)$ & $v_{\rm drift}/\ue$ 
      & $\tau_{\rm V}$ & $\tau_{10}$ & $\tau_{\rm F}$ & $\beta$ \\ \hline \hline
L5\_m & $3 \cdot 10^{-6}$ &  6.142 & 4.74 & 17.22 & 1.17 & 0.97 & ~0.4456 & 0.0097 & 0.0696 & 0.0510 \\
L5\_n &                   &  6.148 & 4.75 & 13.42 & 0.91 & 1.09 & ~0.5474 & 0.0120 & 0.0848 & 0.0398 \\
      & & & & & & & & & \\[-3mm]
L4\_m & $1 \cdot 10^{-5}$ &  6.352 & 4.90 & 20.14 & 1.39 & 0.44 & ~1.6870 & 0.0368 & 0.2407 & 0.1989 \\
L4\_n &                   &  6.381 & 4.93 & 17.17 & 1.19 & 0.48 & ~1.9050 & 0.0416 & 0.2677 & 0.1696 \\
      & & & & & & & & & \\[-3mm]
L3\_m & $3 \cdot 10^{-5}$ &  6.872 & 5.30 & 18.70 & 1.35 & 0.21 & ~5.7730 & 0.1260 & 0.6553 & 0.5540 \\
L3\_n &                   &  6.928 & 5.35 & 15.39 & 1.11 & 0.23 & ~6.4740 & 0.1413 & 0.7115 & 0.4559 \\
      & & & & & & & & & \\[-3mm]
L2\_m & $8 \cdot 10^{-5}$ &  7.822 & 6.04 & 14.46 & 1.11 & 0.10 & 17.8000 & 0.3886 & 1.3980 & 1.1429 \\
L2\_n &                   &  7.925 & 6.12 & 10.42 & 0.80 & 0.12 & 20.7200 & 0.4522 & 1.5330 & 0.8230 \\
      & & & & & & & & & \\[-3mm]
L1\_m & $2 \cdot 10^{-4}$ &  9.256 & 7.14 & 10.24 & 0.85 & 0.03 & 50.5900 & 1.1040 & 2.6950 & 2.0219 \\
L1\_n &                   &  9.530 & 7.36 &  5.08 & 0.43 & 0.08 & 66.4600 & 1.4510 & 3.1720 & 1.0035 \\
                  \hline \hline
\end{tabular} 
\caption[]
{
Same as Tab.~\ref{tab9} but for a Carbon star with $\Mstar=5 \, \Msun, \Lstar=5
\cdot 10^4 \, \Lsun$, and $\Teff=2000$~K.  The velocity structure and resulting
spectral energy distribution for models L5\_m, L3\_m and L1\_m are displayed in
Fig.11.
}
\label{tab11}
\end{center}
\end{table*}
%==============================================================================
\end{document}
