Exploring the Dynamics of CME-Driven Shocks by Comparing Numerical Modeling and Observations

TL;DR

This study combines advanced numerical modeling with multi-messenger observations to understand how CME-driven shocks influence solar energetic particles and gamma-ray emissions, highlighting the importance of detailed background and source region data.

Contribution

It introduces a coupled modeling approach using AWSoM and iPATH to analyze the impact of shock evolution on particle acceleration and gamma-ray production.

Findings

Shock evolution complexity affects SEP spectra.

Accurate background modeling improves understanding of gamma-ray emissions.

Coupled models help interpret observational data.

Abstract

Shocks driven by coronal mass ejections (CMEs) are primary drivers of gradual solar energetic particle (SEP) events, posing significant risks to space technology and astronauts. Concurrently, particles accelerated at these shocks may also propagate back to the Sun, potentially generating gamma-ray emissions through pion decay. We incorporated advanced modeling and multi-messenger observations to explore the role of CME-driven shocks in gamma-ray emissions and SEPs. Motivated by Fermi-LAT long-duration solar flares, we used the AWSoM MHD model to investigate the connection between the shocks and the properties of observed gamma-ray emissions. By coupling the AWSoM with iPATH model, we evaluate the impact of shock evolution complexity near the Sun on SEP intensity and spectra. Our result points to the importance of accurate background coronal and solar wind modeling, as well as detailed observations of CME source regions, in advancing our understanding of CME-driven shocks and the dynamics of associated energetic particles.