Solar irradiance and the solar wind are two key drivers of space weather that modulate the dynamics of Earth’s upper atmosphere. Solar irradiance, particularly in the extreme ultraviolet (EUV) and X-ray wavelengths, directly heats and ionizes the thermosphere and ionosphere, producing variations that follow both the solar cycle and shorter-term solar activity. In parallel, the solar wind interacts with Earth’s magnetic field, driving geomagnetic storms and high-latitude energy inputs that redistribute momentum, heat, and charged particles throughout the upper atmosphere. The Sun’s magnetic field is the fundamental driver behind both solar irradiance variability and solar wind conditions. Understanding this relationship is critical to model and forecast how solar variability affects the Earth’s upper atmosphere. The goal of this work is to understand the interplay between the evolution of the magnetic field, the radiative output of the solar atmosphere and the continuous mass flow from the Sun. These processes will be investigated with a combination of simulations, observations, and models.  

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