All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{8876f1.eps}\end{figure}$ Figure 1: The velocity profile for IK Tau from the dynamical model overlayed with the velocity data obtained from mapping of maser emission (see Bains et al. 2003, and references therein). H₂O masers (circles) and OH maser (squares) have been used. The expansion velocity derived from the CO data is marked by a diamond.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18.5cm]{8876f2.eps}\end{figure}$ Figure 2: ${\rm\chi ^{2}}$ -maps showing the level of consistency between the velocity-integrated CO line intensity from the observations and the line model when varying the mass-loss rate and the h-parameter. The innermost contour corresponds to a 68% confidence level. The star indicates the best-fit model. The shapes of the line profiles were taken into account when choosing the best-fit model.
Open with DEXTER

In the text

$\begin{figure} {\includegraphics[width=18.5cm]{8876f3.eps} } \end{figure}$ Figure 3: The observed CO $J = 1 \rightarrow 0$ line from OSO and the $2 \rightarrow 1$ , $3 \rightarrow 2$ , $4\rightarrow 3$ , and $6\rightarrow 5$ lines from JCMT (histogram) of the carbon star LP And, overlayed with the best-fit model ( $\dot{M} =7 \times 10 ^{-6}~M_{\odot}$ yr^-1) lines (solid line) from the radiative transfer modelling. The reduced $\chi ^{2}$ for this model is 0.25. See Sect. 8.1.1.
Open with DEXTER

In the text

$\begin{figure} {\includegraphics[width=15.1cm]{8876f4.eps} } \end{figure}$ Figure 4: The observed CO $J = 1 \rightarrow 0$ line from OSO and the $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT (histogram) of the M-type star TX Cam, overlayed with the best-fit model ( $\dot{M} =7 \times 10 ^{-6}~M_{\odot}$ yr^-1) lines (solid line) from the radiative transfer modelling. The reduced $\chi ^{2}$ for this model is 3.0. See Sect. 8.2.1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{8876f5.eps}\end{figure}$ Figure 5: $\chi ^{2}$ -maps showing the level of consistency between the photometric fluxes and the dust-continuum model when varying $\tau_{10~\mu {\rm m}}$ and $T_{{\rm d}}$ , at constant $T_{{\rm eff}}$ . The innermost contour corresponds to a 68% confidence level. The star indicates the best-fit model chosen using the strategy described in Sect. 7.2.1. All grids are terminated at $T_{\rm d}(r_{\rm i}) = 1500$ K since a dust temperature at the inner radius larger than this is unlikely. This determines the best-fit models in the cases of CW Leo and AFGL 3068.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{8876f6.epsi}\\ [2mm] \inc... ...876f7.epsi}\\ [2mm] \includegraphics[width=18cm,clip]{8876f8.epsi}\end{figure}$ Figure 6: Observed photometric fluxes together with ISO-LWS and ISO-SWS spectra overlayed by the best-fit model SEDs derived from the dust radiative transfer model. The model is represented by the solid line in all panels. The dashed line shows the model SED when the interstellar extinction is not taken into account. The ISO-LWS spectra are plotted for all stars but GX Mon. The lower panels show the wavelength interval 5-35 $\mu$ m in more detail for the M-type stars. The best-fit models are here shown together with the observed IRAS-LRS spectra (dotted line) and the ISO-SWS spectra (dot-dashed line) when available.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8876f9.eps}\end{figure}$ Figure 7: Comparing the mass-loss-rate results from the CO model and the dynamical model. Dots mark the M-type stars, and squares the carbon stars. The full drawn line represents a one-to-one relation and the dashed lines subtend the range within a factor of 3.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=7cm,angle=-90]{8876f10.eps}\end{figure}$ Figure 8: Observed line intensity ratios for the sample sources (squares) compared with predictions from the standard model for various mass-loss rates (stars).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm]{8876f11.eps}\end{figure}$ Figure A.1: Mass-loss rates derived using Eq. (A.1) and the parameters in Table A.1 versus the mass-loss rates estimated using the Monte Carlo model for the same stars. Red triangles represent carbon stars, blue squares, M-type stars, and green dots represent S-type stars.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15.0cm,clip]{8876f12.eps}\end{figure}$ Figure C.1: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the carbon star CW Leo, overlayed with the best-fit model ( $\dot{M} =2 \times 10 ^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.6$ . See Sect. 8.1.2.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=15.0cm]{8876f13.eps} } \end{figure}$ Figure C.2: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the carbon star RW LMi, overlayed with the best-fit model ( $\dot{M} = 5 \times 10 ^{-6}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=2.1$ . See Sect. 8.1.5.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=15.0cm]{8876f14.eps} } \end{figure}$ Figure C.3: The observed CO $J = 1 \rightarrow 0$ line from OSO, 2 $\rightarrow$ 1, $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the carbon star V384 Per, overlayed with the best-fit model ( $\dot{M} = 3 \times 10 ^{-6}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=3.7$ . See Sect. 8.1.3.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=18.5cm]{8876f15.eps} } \end{figure}$ Figure C.4: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , $4\rightarrow 3$ , and $6\rightarrow 5$ lines from JCMT, of the carbon star AFGL 3068, overlayed with the best-fit model ( $\dot{M}=2~\times~10^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.7$ . See Sect. 8.1.4.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=15.0cm]{8876f16.eps} } \end{figure}$ Figure C.5: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the M-type star GX Mon, overlayed with the best-fit model ( $\dot{M} =2 \times 10 ^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.04$ . See Sect. 8.2.2.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=18.5cm]{8876f17.eps} } \end{figure}$ Figure C.6: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , $4\rightarrow 3$ , and $6\rightarrow 5$ lines from JCMT, of the M-type star WX Psc, overlayed with the best-fit model ( $\dot{M}=4\times10^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=1.0$ , when the $6\rightarrow 5$ line is omitted. See Sect. 8.2.3.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=15.0cm]{8876f18.eps} } \end{figure}$ Figure C.7: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the M-type star IK Tau, overlayed with the best-fit model ( $\dot{M} =1 \times 10 ^{-5}~M _\odot$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.5$ . See Sect. 8.2.4.
Open with DEXTER

In the text

$\begin{figure}{\includegraphics[width=15.0cm]{8876f19.eps} } \end{figure}$ Figure C.8: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , 3 $\rightarrow$ 2, and $4\rightarrow 3$ lines from JCMT, of the M-type star IRC-10529, overlayed with the best-fit model ( $\dot{M}=1.6\times 10^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=4.6$ . See Sect. 8.2.5.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8876f1.eps}\end{figure}$	Figure 1: The velocity profile for IK Tau from the dynamical model overlayed with the velocity data obtained from mapping of maser emission (see Bains et al. 2003, and references therein). H₂O masers (circles) and OH maser (squares) have been used. The expansion velocity derived from the CO data is marked by a diamond.
Open with DEXTER

$\begin{figure} {\includegraphics[width=15.1cm]{8876f4.eps} } \end{figure}$	Figure 4: The observed CO $J = 1 \rightarrow 0$ line from OSO and the $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT (histogram) of the M-type star TX Cam, overlayed with the best-fit model ( $\dot{M} =7 \times 10 ^{-6}~M_{\odot}$ yr^-1) lines (solid line) from the radiative transfer modelling. The reduced $\chi ^{2}$ for this model is 3.0. See Sect. 8.2.1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8876f9.eps}\end{figure}$	Figure 7: Comparing the mass-loss-rate results from the CO model and the dynamical model. Dots mark the M-type stars, and squares the carbon stars. The full drawn line represents a one-to-one relation and the dashed lines subtend the range within a factor of 3.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,height=7cm,angle=-90]{8876f10.eps}\end{figure}$	Figure 8: Observed line intensity ratios for the sample sources (squares) compared with predictions from the standard model for various mass-loss rates (stars).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm]{8876f11.eps}\end{figure}$	Figure A.1: Mass-loss rates derived using Eq. (A.1) and the parameters in Table A.1 versus the mass-loss rates estimated using the Monte Carlo model for the same stars. Red triangles represent carbon stars, blue squares, M-type stars, and green dots represent S-type stars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15.0cm,clip]{8876f12.eps}\end{figure}$	Figure C.1: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the carbon star CW Leo, overlayed with the best-fit model ( $\dot{M} =2 \times 10 ^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.6$ . See Sect. 8.1.2.
Open with DEXTER

$\begin{figure}{\includegraphics[width=15.0cm]{8876f13.eps} } \end{figure}$	Figure C.2: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the carbon star RW LMi, overlayed with the best-fit model ( $\dot{M} = 5 \times 10 ^{-6}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=2.1$ . See Sect. 8.1.5.
Open with DEXTER

$\begin{figure}{\includegraphics[width=15.0cm]{8876f14.eps} } \end{figure}$	Figure C.3: The observed CO $J = 1 \rightarrow 0$ line from OSO, 2 $\rightarrow$ 1, $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the carbon star V384 Per, overlayed with the best-fit model ( $\dot{M} = 3 \times 10 ^{-6}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=3.7$ . See Sect. 8.1.3.
Open with DEXTER

$\begin{figure}{\includegraphics[width=15.0cm]{8876f16.eps} } \end{figure}$	Figure C.5: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the M-type star GX Mon, overlayed with the best-fit model ( $\dot{M} =2 \times 10 ^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.04$ . See Sect. 8.2.2.
Open with DEXTER

$\begin{figure}{\includegraphics[width=15.0cm]{8876f18.eps} } \end{figure}$	Figure C.7: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , $3 \rightarrow 2$ , and $4\rightarrow 3$ lines from JCMT, of the M-type star IK Tau, overlayed with the best-fit model ( $\dot{M} =1 \times 10 ^{-5}~M _\odot$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=0.5$ . See Sect. 8.2.4.
Open with DEXTER

$\begin{figure}{\includegraphics[width=15.0cm]{8876f19.eps} } \end{figure}$	Figure C.8: The observed CO $J = 1 \rightarrow 0$ line from OSO, $2 \rightarrow 1$ , 3 $\rightarrow$ 2, and $4\rightarrow 3$ lines from JCMT, of the M-type star IRC-10529, overlayed with the best-fit model ( $\dot{M}=1.6\times 10^{-5}~M_{\odot}$ yr^-1) from the CO radiative transfer modelling. The reduced $\chi ^{2}$ for this model is $\chi ^{2}_{\rm {red}}=4.6$ . See Sect. 8.2.5.
Open with DEXTER