Modelling Supernova Explosions in Disk Galaxy Simulations

Le résumé fourni par la source

We present an enhanced model for disk galaxy simulations that better incorporates supernova (SN) feedback in a non-uniform interstellar medium (ISM). Current models often oversimplify ISM structure by considering a homogeneous medium, compromising the accuracy of energy and momentum transfer from supernova events. Our approach implements locally calculated radial density profiles that follow a power law, capturing the heterogeneous nature of the ISM. The model calculates density gradients across radial scales to realistically simulate how supernova shocks propagate through varying environments. This methodology creates a more physically accurate representation of the interactions between stellar feedback and ISM structure. We evaluate various density profile parameters to determine their effects on the ISM. By integrating these locally resolved profiles into our multi-scale framework, we achieve improvements in physical accuracy while maintaining computational efficiency. Our simulations show enhanced ability to reproduce observed galactic features, including realistic star formation rates and outflow characteristics. This work improves the treatment of supernova explosions in non-uniform media and allows for more reliable predictions about galaxy formation and evolution processes, bridging the gap between theoretical models and observations.

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