# Nonlinear Evolution of Ion Kinetic Instabilities in the Solar Wind

## TL;DR

This study uses a novel 3D hybrid model to investigate the nonlinear evolution of ion kinetic instabilities in the solar wind, revealing their role in heating and magnetic fluctuation dissipation near the Sun.

## Contribution

First application of a 3D hybrid PIC-fluid model to simulate ion kinetic instabilities in the solar wind, capturing nonlinear evolution and dissipation processes.

## Key findings

- Self-consistent non-Maxwellian ion VDFs produced
- Temperature anisotropies observed in unstable ion populations
- Wave spectra consistent with solar wind observations

## Abstract

In-situ observations of the solar wind (SW) plasma from 0.29 to 1AU show that the protons and alpha particles are often non-Maxwellian, with evidence of kinetic instabilities, temperature anisotropies, differential ion streaming, and associated magnetic fluctuations spectra. The kinetic instabilities in the SW multi-ion plasma can lead to preferential heating of alpha particles and the dissipation of magnetic fluctuation energy, affecting the kinetic and global properties of the SW. Using for the first time a three-dimensional hybrid model, where ions are modeled as particle using the Particle-In-Cell (PIC) method and electrons are treated as fluid, we study the onset, nonlinear evolution and dissipation of ion kinetic instabilities. The Alfven/ion-cyclotron, and the ion drift instabilities are modeled in the region close to the Sun (~10R_s). Solar wind expansion is incorporated in the model. The model produces self-consistent non-Maxwellian velocity distribution functions (VDFs) of unstable ion populations, the associated temperature anisotropies, and wave spectra for several typical SW instability cases in the nonlinear growth and saturation stage of the instabilities. The 3D hybrid modeling of the multi-ion SW plasma could be used to study the SW acceleration region close to the Sun that will be explored by the Parker Solar Probe mission.