# Simulating the interaction of a non-magnetized planet with the stellar wind produced by a sun-like star using the FLASH Code

## TL;DR

This paper adapts the FLASH simulation code to model the interaction of a non-magnetized, atmosphere-less planet with stellar wind, analyzing density, magnetic, and velocity patterns, and assessing viscosity effects.

## Contribution

It introduces a novel extension of the FLASH code to simulate rigid bodies in MHD scenarios, specifically for non-magnetized planets interacting with stellar wind.

## Key findings

- Density, magnetic field, and velocity patterns around the planet characterized.
- Viscosity influences the flow and magnetic field configurations.
- An improved simulation methodology is proposed for future studies.

## Abstract

The study of the interaction between solid objects and magnetohydrodynamic (MHD) fluids is of great importance in physics as consequence of the significant phenomena generated, such as planets interacting with stellar wind produced by their host stars. There are several computational tools created to simulate hydrodynamic and MHD fluids, such as the FLASH code. In this code there is a feature which permits the placement of rigid bodies in the domain to be simulated. However, it is available and tested for pure hydrodynamic cases only. Our aim here is to adapt the existing resources of FLASH to enable the placement of a rigid body in MHD scenarios and, with such a scheme, to produce the simulation of a non-magnetized planet interacting with the stellar wind produced by a sun-like star. Besides, we consider that the planet has no significant atmosphere. We focus our analysis on the patterns of the density, magnetic field and velocity around the planet, as well as the influence of the viscosity on such patterns. At last, an improved methodological approach is available to other interested users.