Dr
Nicolas
Peschken
University of Florence, Italy
Cosmic rays are high-energy charged particles, primarily protons and electrons, that are produced and accelerated to relativistic speeds in the remnants of supernovae. These particles dynamically interact with the gas in the interstellar medium, transferring momentum and energy, which can accelerate vast amounts of gas and generate powerful galactic winds. While this mechanism is highly effective at driving large-scale outflows in massive galaxies, it is often overlooked in current galaxy models.
In this colloquium, we will explore the role of cosmic rays in shaping galactic winds by employing magneto-hydrodynamical simulations of Milky Way-like galaxies. These simulations will include supernova feedback in the form of both thermal and cosmic ray energy injections. By comparing models with purely thermally-driven outflows to those incorporating cosmic rays, we will highlight the critical influence of cosmic rays on galactic winds. Additionally, we will discuss how this research could enhance our understanding of wind dynamics and composition in our own Galaxy.
This is a hybrid event:
Room D, the Institute of Physics PAS, Al. Lotników 32/46
Online: Zoom Link, (Passcode: 134595, Meeting ID: 823 8038 0442)
