Modeling of Coronal Mass Ejection Originating from a Sheared Arcade of Realistic Active-region Scale and Its Propagation in the Heliosphere: Methodology

Abstract Simulating coronal mass ejections (CMEs) from their origin in active regions (ARs) to their propagation to Earth remains challenging, particularly when aiming to resolve AR scales and employ realistic magnetic field strengths without compromising computational efficiency. Here we present a methodology for end-to-end CME modeling that addresses these challenges. Three nested magnetohydrodynamic simulations are coupled to jointly cover the heliosphere from the solar surface to beyond 1.5 au. A block-structured adaptive mesh refinement scheme is employed to achieve ∼700 km resolution in the low corona, allowing AR scales to be resolved while maintaining the total grid count below 10 8 across the entire computational domain. A semirelativistic Boris correction combined with a relativistic mass-density factor is used to handle magnetic field strengths up to 10 3 G without prohibitively small time steps. Using this model, we simulate the emergence of a bipolar AR into the corona, the initiation of a CME by shearing of the AR core field, and the subsequent evolution. Our simulation captures its pre-eruption energy buildup, triggered by magnetic reconnection, rapid acceleration, and propagation to 1 au and beyond. The simulated CME exhibits a three-part structure in synthetic coronagraph images and a torus-shaped flux rope in the heliosphere, with synthetic in situ observations showing shock formation, density compression, and a prolonged southward B z component at 1 au. The entire simulation requires about 1 day on a moderately sized cluster (e.g., 600 processors), while the simulated CME takes 3 days to arrive at 1 au, offering a lead time of 2 days if used for forecasting.