![\begin{figure}
\par\includegraphics[width=8.2cm,clip]{h4634_f1.eps}\end{figure}](/articles/aa/full/2003/41/aah4634/img23.gif) |
Figure 1:
Upper panel:
The volume integrated cooling rates over the spherical shell
due to various cooling mechanisms are shown as a function of r in log scales.
The
 's are in
 .
Lower panel:
The relative electron temperature differences are shown
as a function of r.
The relative electron temperature difference is defined as
(T0-T*)/T0,
where T0 is the electron temperature of
the case without the stellar cooling.
The thin and thick solid curves represent
the cases when the cooling star is at
 and
 ,
respectively.
The dotted curve and the dashed curve represent volume-integrated cooling rate
due to synchrotron cooling and
bremsstrahlung cooling, respectively. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.4cm,clip]{h4634_f2.eps}\end{figure}](/articles/aa/full/2003/41/aah4634/img35.gif) |
Figure 2:
Upper panel:
We show the radio spectra of the ADAFs without stellar cooling by
the solid curve, with stellar cooling at the pericenter
by the dotted curve and at the apocenter by the dashed curve.
Note that all the curves are indistinguishable at this scale.
The luminosity in
and
the frequency in Hz are shown in the log scale.
Lower panel: The relative difference of
the radio spectrum at two different epochs is shown. |
| Open with DEXTER | |
In the text