Speaker
Description
The Large Magellanic Cloud (LMC) induces a significant time-dependent gravitational perturbation on the Milky Way dark matter halo, altering the local phase-space distribution of dark matter in the Solar neighborhood. Cosmological simulations that sample potential Milky Way formation histories provide a powerful framework to characterize the dynamical response of the halo to such a massive satellite interaction. In this talk, I will discuss the imprint of the LMC-Milky Way system on the local dark matter distribution using state-of-the-art cosmological simulations. I will then discuss the consequences of these non-equilibrium features for dark matter phenomenology, including their impact on both standard and non-standard interaction models, spanning light and heavy dark matter scenarios.