  I report a coronal wave observed in Fexii, soft X-ray, and Halpha on November
6, 2006, jointly with a CME and a flare to show the spatial and temporal
relation of the wave and the CME. I also take advantage of the spectral
resolution of the wave to obtain an approximation of its temperature. Finally,
I compare the magnetic field topology to the wave location. The observations in
two band passes show bright fronts that are co-spatial when observed at the
same time, therefore I believe that the same wave is observed in different band
passes. The wave front is not observable in Halpha, but just in Fexii and in
soft X-ray, indicating that the temperature of the wave front is slightly
higher than the chromospheric temperature. The ratio of emission through two
SXI filters gives a temperature of 7 10^6 K for the wave front. The
northern-most edge of the CME footprint related to this wave corresponds to the
last location of the wave on the limb. The image processing reveals stationary
brightenings produced on the passage of the wave front. The potential spherical
extrapolation of the sun shows that those stationary brightenings are lying in
jumps of magnetic field lines connectivity.
