Speaker
Description
The self-similar spherical collapse model provides an insightful framework for understanding the formation and evolution of galaxy clusters in an expanding Universe. However, cosmological simulations have revealed significant deviations of the cluster outskirts and their evolution from the self-similar prediction. In this talk, I will discuss intriguing physics behind this problem and introduce our novel idealized simulations designed to understand structures in the outskirts of galaxy clusters, including dark matter splashback, accretion shocks, and etc. Our findings indicate distinguished behaviors of the gas and dark matter boundaries driven by merger processes. I will further discuss the concept of total and smooth mass accretion rates and their role in determining the cluster boundaries.
