Plasma Mechanism of Radio Emission Generation on a Shock Wave in the Vicinity of an Exoplanet

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Abstract

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.

About the authors

A. A. Kuznetsov

Gaponov-Grekhov Institute of Applied Physics RAS

Email: kuznetsov.alexey@ipfran.ru
Nizhny Novgorod, Russia

V. V. Zaitsev

Gaponov-Grekhov Institute of Applied Physics RAS

Nizhny Novgorod, Russia

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