This study evaluates the possibility of efficient radio emission generation in the bow shock region of hot Jupiter–type exoplanets. As a source of energetic electrons, the shock drift acceleration mechanism at a quasi-perpendicular shock is proposed. Electrons reflected and accelerated by the shock propagate through the relatively dense stellar wind plasma and excite plasma waves; therefore, a plasma emission mechanism is considered as the source of the resulting radio waves. Using the bow shock of the hot Jupiter HD~189733b as a case study, the properties of the energetic electron beam, the excited plasma waves, and the resulting radio frequencies are estimated. An energy-based analysis is carried out to identify the range of stellar wind parameters for which radio emission from the bow shock of the exoplanet HD~189733b could be detectable by modern astronomical instruments.
A. A. Kuznetsov (Wed,) studied this question.