Synchrotron emission from circumstellar disks around massive stars

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 $L_s\sim {10}^{-5}\text{lsun}$ for a central star with $\dot{M}={10}^{-6}\text{msun}$ yr${}^{-1}$, comparable with the value observed around the TW object in the W3(OH) region.