Synchrotron emission from circumstellar disks around massive stars

Abstract

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.

arXiv comment7 pages, no figs, accepted in A&A

References in corpus (10)

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Cited by in corpus (7)

• Core fragmentation and Toomre stability analysis of W3(H2O): A case study of the IRAM NOEMA large program CORE
• Deciphering the ionized gas content in the massive star forming complex G75.78+0.34
• Methanol in W3(H2O) and Surrounding Regions
• Non-thermal emission from cosmic rays accelerated in HII regions
• Parameter study for the burst mode of accretion in massive star formation
• Infrared Excess of a Large OB Star Sample
• Model of the W3(OH) environment based on data for both maser and 'quasi-thermal' methanol lines