Abstract. When a process of magnetic reconnection takes place in the solar corona, the magnetic field lines are rearranged and the relaxation of the new configuration can shoot plasma away from this site. While propagating further in the corona, the newly formed plasma jets create disturbances in the background medium. Such configuration can lead to the excitation of electrostatic waves that are expected to be highly instable in general sense. Here, the conditions for generation of such electrostatic instability is studied using a multifliud approach. The propagation of plasma jets through the solar corona could be one of the possible trigger mechanisms for the generation of electrostatic instability that later on could lead to energization (heating and/or acceleration) of electrons in the solar corona.

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