The Sun is a main-sequence, G-type star. Traditionally, stellar astrophysics does not account much for the detailed information we have gathered about the Sun, the solar corona, and the solar wind in the last few decades. My philosophy in my research about stellar astrophysics is to implement the detailed physics we know about the Sun to other stars in order to investigate when and how this detailed physics matters. I use a magnetohyrodynamic (MHD) model that includes the detailed physics of the solar corona to study stellar coronae of other stars with hot corona and thermally-driven stellar wind (stellar wind that is driven by the pressure gradient between the star and space).
The main focus of my stellar astrophysical research is to study mass-loss rates of solar analogs and how do changes in stellar rotation, magnetic activity, and magnetic complexity affect the stellar mass-loss to the stellar wind? Such a modeling work can constrain stellar mass-loss rates as stellar winds of cool stars cannot be directly measured (they are too week). It is important to determine these mass-loss rates since they determine the rate of spindown of stars over time in stellar evolution models.
The stellar corona of AB Doradus:
Stellar mass loss rates as a function of rotation period (Cohen & Drake 2014):
