| Abstract : | Relativistic magnetic reconnection is thought to be one of the key processes involved
in the acceleration of charged particles, which results in the emission of synchrotron radiation
and electromagnetic radiation, a phenomenon observed in celestial objects
like pulsar wind nebulae, gamma-ray bursts, and powerful jets. These phenomena
are characterized by their highly nonlinear and multi-scale nature, which needs simulation
power to overcome the analytical challenges. Here, we present the results of a
relativistic magnetic reconnection simulation initiated by configuring a Harris sheet,
a common setup for exploring magnetic reconnection. For our simulation, we used
the Black Hole Accretion Code (BHAC), which is a multidimensional general relativistic
magnetohydrodynamic code made for modeling complex astrophysical processes. We
studied the Alfven four Mach number and reconnection rate evolution over a time
period for this system. By examining this, we gain an understanding of the interplay
between magnetic fields and plasma in a relativistic regime. Then we obtain
the Sweet-Parker scaling by calculating the reconnection rate at different Reynolds
number. Resolution studies are done to check for the convergence of reconnection rates. Our results are in agreement with the findings previously reported in the
literature. |
