Nonthermal radio emission from hot star winds

Abstract

Nonthermal radio emission has been observed from some of the most luminous hot star winds. It is understood to be synchrotron radiation of the relativistic electrons in the winds. To understand how the electrons are accelerated to such high energies and to correctly explain the observed radio flux and spectra require an exhaustive investigation of all the relevant physical processes involved and possibly point to a complex wind structure. In this paper we discuss the logical path toward a comprehensive model of the nonthermal radio emission from hot star winds. Based on the available observational data and fundamental theoretical considerations, we found that the only physically viable and self-consistent scenario is:the nonthermal radio emission is synchrotron radiation of relativistic electrons ⇄ the electrons are accelerated by shocks via the first-order Fermi mechanism ⇄ the acceleration has to be in situ in the radio emitting region ⇄ the shocks formed at the base of the winds have to propagate to beyond the radio photosphere).