# Two-fluid numerical simulations of the origin of the fast solar wind

## TL;DR

This study uses advanced 2.5D simulations with the JOANNA code to model plasma outflows from the solar surface, providing insights into the origin of the fast solar wind by matching observed mass and energy loss rates.

## Contribution

The paper introduces realistic 2.5D numerical simulations of plasma outflows using the JOANNA code, linking solar granulation dynamics to the fast solar wind origin.

## Key findings

- Simulated outflows match observed mass and energy loss rates.
- Outflows originate from the upper chromosphere, transition region, and inner corona.
- Results support the hypothesis that solar granulation drives the fast solar wind.

## Abstract

With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities consistent to the order of magnitude with the observational findings for mass and energy losses in the upper chromosphere, transition region and inner corona, and they may originate the fast solar wind.