  We report the discovery of variability in the X-ray emission from the
Wolf-Rayet type star WR 65. Using archival Chandra data spanning over 5 yr we
detect changes of the X-ray flux by a factor of 3 accompanied by changes in the
X-ray spectra. We believe that this X-ray emission originates from wind-wind
collision in a massive binary system. The observed changes can be explained by
the variations in the emission measure of the hot plasma, and by the different
absorption column along the binary orbit. The X-ray spectra of WR 65 display
prominent emission features at wavelengths corresponding to the lines of
strongly ionized Fe, Ca, Ar, S, Si, and Mg. WR 65 is a carbon rich WC9d star
that is a persistent dust maker. This is the first investigation of any X-ray
spectrum for a star of this spectral type. There are indications that the dust
and the complex geometry of the colliding wind region are pivotal in explaining
the X-ray properties of WR 65.
