Tests of a new code that simulates the evolution of solar winds and CMEs

Abstract

AbstractWe present the tests of a new code that solves Euler equations in three dimensions used to simulate the dynamics of the Solar Wind. The code is based on a finite volume discretization and uses high resolution shock capturing methods, with second order variable reconstructors and approximate flux formulae of the HLL class. It uses Cartesian coordinates and fixed mesh refinement. The equations are written in flux balance law form, which allows the evolution of conservative variables. The evolution is carried out using the method of lines with second order time integration. For the simulation of a solar wind we assume the Sun lies at the coordinate origin, and inject the fluid variables through the surface of a lego-sphere with radius 20R⊙, where all the characteristic speeds point outwards from the solar surface. We manage to obtain stationary winds that reproduce winds of literature in terms of density, velocity and temperature of the plasma. On top of the stationary wind it is possible to launch Coronal Mass Ejections (CMEs) that propagate through the stationary Solar Wind from the injection surface all the way to the Earth. Finally, in order to incorporate the role of orbiting satellites that monitor Solar Winds and CMEs, the code also measures wind variables at detector locations on their actual trajectories around the Sun.