  We argue that the interaction of stellar wind with the surface of a
circumstellar accretion (or protoplanetary) disk can result in the acceleration
of relativistic electrons in an external layer of the disk, and produce
synchrotron radiation. Conservative estimates give a total synchrotron
luminosity $L_s\sim 10^{-5}\lsun$ for a central star with $\dot M=10^{-6}\msun$
yr$^{-1}$, comparable with the value observed around the TW object in the
W3(OH) region.
