On magnetohydrodynamic reconnection in relativistic plasmas

Black holes and neutron stars posses extremely large mass densities and extremely strong gravitational fields, while being surrounded by plasma.
Flares are highly explosive events observed on relatively small scales within the jets and accretion disc (corona) of compact astrophysical objects.
These high-energy flares release large amounts of magnetic energy causing non-thermal particle acceleration up to relativistic speeds.
Magnetic reconnection causes magnetic energy to convert into kinetic energy and thermal energy of the plasma leading to possibly relativistic particle speeds.
Reconnection is due to resistivity causing magnetic energy to dissipate to microscopic length scales and it being transferred to particles.
On these scales, reconnection typically causes the formation of plasmoids, containing high-energy particles, which are able to grow and power the high-energy flares.
The goal is to resolve the long-term high Lundquist number dynamics of an idealized double current sheet system using relativistic magnetohydrodynamics showing secondary tearing events and plasmoid coalescence.