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 Alfvén 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.
Highlights
The origin of the solar wind is one of the most important unsolved problems in heliophysics
We report some recent progress in the understanding of how the electron beams accelerated by nanoflares shape the solar wind non-thermal electron velocity distribution function (VDF), generate kinetic waves, and produce nano-Type III radio bursts
We have shown that nanoflare-accelerated electron beams can trigger electron two-stream instability (ETSI), which generates kinetic turbulence as well as a non-Maxwellian electron VDF, consistent with observations of the solar wind [4]
Summary
The origin of the solar wind is one of the most important unsolved problems in heliophysics. The concept of solar wind and the first steady hydrodynamic solar wind model were proposed by Parker in 1958 [1]. The Parker model describes the solar wind as a continuous plasma outflow from the solar corona, maintained by the stationary expansion of the Sun’s atmosphere. As pointed out by Parker in 1965 [2], the steady solar wind model only concerns the general dynamical principles but the solar corona is actively heated to maintain the outflow. With the help of more and more powerful computer simulations, it has become possible to reach a better understanding of the detailed physical processes in the solar corona and how these processes affect the properties of the solar wind [3, 4, 5, 6, 7, 8, 9, 10, 11]. We report some recent progress in the understanding of how the electron beams accelerated by nanoflares shape the solar wind non-thermal electron velocity distribution function (VDF), generate kinetic waves, and produce nano-Type III radio bursts
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