Deflexión de eyecciones coronales de masa: Simulaciones numéricas

Coronal mass ejections (CMEs) are eruptive events in which large amounts of solar mass are released, dragging magnetic fields stronger than those in the environment and expanding into the interplanetary medium. It is known that not all CMEs are ejected radially and deflections may be due to the influence of magnetic structures surrounding the formation area of the ejection, particularly coronal holes. The present contribution studies the evolution of CMEs through numerical simulations. Different magnetic scenarios are simulated to systematically analyze how the different properties of the coronal hole can contribute to the deflection of CMEs, in the early stages of their evolution.