Relativistic Magnetic reconnetion in Atrophysical Plasmas

Astrophysical compact objects like neutron stars and black holes are surrounded by a hot gas of charged particle known as plasma. In these environments, we observe powerful phenomena, including pulsar wind nebulae, jets, and gamma-ray bursts. The mechanisms behind particle acceleration and high-energy emissions, particularly magnetic reconnection, are not fully understood. Magnetic reconnection, where magnetic field lines break and reconnect, is believed to drive particle acceleration up to ultra-relativistic speeds, but its detailed dynamics remain largely unexplored.Recent advancements in simulation techniques and observational capabilities make this an opportune moment to resolve key questions in high-energy plasma physics. This project will investigate relativistic magnetic reconnection and its role in particle acceleration and radiation production using advanced simulation methods, including Particle-in-Cell (PIC) simulations for kinetic modeling. The ECsim code will explore the initiation of magnetic reconnection, while the TRISTAN-v2 code will incorporate photon interactions and pair production. Alongside these simulations, an analytical model will be developed to predict reconnection timescales and verify the simulation results. These tools will study the onset of reconnection, particle trajectories, and the effects of radiative cooling, providing new insights into high-energy astrophysical processes.