« An inside out view of the coronae and winds of cool stars »
Cool stars, like our Sun, produce powerful stellar winds that shape their evolution and influence the atmospheres of orbiting planets. While the solar wind is well studied, our understanding of winds from other cool stars remains limited due to the challenges of direct observation. In this talk, I will present results from state-of-the-art 3D magnetohydrodynamic (MHD) simulations that model stellar winds across a range of F, G, K, and M stars. By analyzing their large-scale magnetic field distributions, I quantify stellar wind properties and explore how they shape the Alfvén surface, a key region for star-planet magnetic interactions. Additionally, I will discuss some insights into coronal abundance patterns in cool stars. While low-activity stars typically show the First Ionization Potential (FIP) effect, highly active M dwarfs exhibit an inverse FIP (iFIP) effect. Using XMM-Newton observations, I investigate whether moderately active M dwarfs follow this trend.