  Colliding Wolf-Rayet (WR) winds produce thermal X-ray emission widely
observed by X-ray telescopes. In wide WR+O binaries, such as WR 140, the X-ray
flux is tied to the orbital phase, and is a direct probe of the winds'
properties. In the Galactic center, $\sim$30 WRs orbit the super massive black
hole (SMBH) within $\sim$10", leading to a smorgasbord of wind-wind collisions.
To model the X-ray emission of WR 140 and the Galactic center, we perform 3D
hydrodynamic simulations to trace the complex gaseous flows, and then carry out
3D radiative transfer calculations to compute the variable X-ray spectra. The
model WR 140 RXTE light curve matches the data well for all phases except the
X-ray minimum associated with periastron, while the model spectra agree with
the RXTE hardness ratio and the shape of the Suzaku observations throughout the
orbit. The Galactic center model of the Chandra flux and spectral shape match
well in the region r$<$3", but the model flux falls off too rapidly beyond this
radius.
