![\begin{figure}
\par\includegraphics[angle=-90,width=7.8cm,clip]{09669fig01.ps}\end{figure}](/articles/aa/full/2008/30/aa09669-08/img31.gif) |
Figure 1:
The electron energy as a function of
(
 )
for different values of energy at t=0 s
(50 keV, 100 keV, 200 keV...6400 keV). The solid lines show the exact, but implicit solutions to
Eq. (1), i.e. Eq. (5).
The dotted lines are the non-relativistic solutions to Eq. (1),
i.e. Eq. (4). |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[angle=-90,width=8cm,clip]{09669fig02.ps}\end{figure}](/articles/aa/full/2008/30/aa09669-08/img44.gif) |
Figure 2:
Low energy electron cosmic rays as expected from first order
Fermi acceleration, including the effects of Coulomb losses (Eq. (9)). The solid line gives the expected spectrum near the shock front,
whereas the other lines show the models for different values of
. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[angle=-90,width=8.2cm,clip]{09669fig03a.ps}\includegraphics[angle=-90,width=8.2cm,clip]{09669fig03b.ps}\end{figure}](/articles/aa/full/2008/30/aa09669-08/img51.gif) |
Figure 3:
Left: spectral energy distribution of Cas A, as measured with
BeppoSAX-PDS (Vink et al. 2001, red) and INTEGRAL-IBIS (Renaud et al. 2006b, green),
assuming a magnetic field of   G, a spectral energy index
of -2.56 (corresponding to a radio-spectral index of
 ),
and a background plasma with
 cm-3.
The bremsstrahlung spectra were calculated
using the analytic cross sections of Haug (1997).
The model spectra are shown for
and
 cm-3 s ( from top to bottom).
Right: spectral energy distribution of Tycho's SNR, as measured by the
BeppoSAX-PDS. The theoretical curves are for  G,
 ,
and
 cm-3. The different curves are
for
 cm-3 s. |
| Open with DEXTER | |
In the text