How Nanoflares Produce Kinetic Waves, Nano-Type III Radio Bursts, and Non-Thermal Electrons in the Solar Wind

TL;DR

This paper investigates how nanoflares accelerate electron beams that induce kinetic waves and radio bursts in the solar wind, providing insights into the origin of non-thermal electrons and solar radio emissions.

Contribution

It presents a simulation and theoretical model showing nanoflare-accelerated electrons generate kinetic waves and radio bursts, linking small-scale solar events to observed solar wind phenomena.

Findings

Nanoflare-accelerated electron beams trigger electron two-stream instability.

Generation of kinetic Alfvén and whistler waves observed.

Model reproduces characteristics of Type III, J, and V solar radio bursts.

Abstract

Observations of the solar corona and the solar wind discover that the solar wind is unsteady and originates from the impulsive events near the surface of the Sun's atmosphere. How solar coronal activities affect the properties of the solar wind is a fundamental issue in heliophysics. We report a simulation and theoretical investigation of how nanoflare accelerated electron beams affect the kinetic-scale properties of the solar wind and generate coherent radio emission. We show that nanoflare-accelerated electron beams can trigger a nonlinear electron two stream instability, which generates kinetic Alfv\'en and whistler waves, as well as a non-Maxwellian electron velocity distribution function, consistent with observations of the solar wind. The plasma coherent emission produced in our model agrees well with the observations of Type III, J and V solar radio bursts. Open questions in the kinetic solar wind model are also discussed.