Speaker
Description
In magnetized astrophysical plasma magnetic reconnection is the accepted mechanism that heats and accelerates plasmoids and affects the dynamics of the plasma. This is thought to be the mechanism for the dissipation of magnetic energy in the still poorly understood phenomena of solar flares, magnetic substorms in the Earth magnetosphere, jets, and relativistic ejections from the accretion discs of compact objects. In this work, we study energy dissipation by solving the Orszag-Tang test problem with different resolutions and numerical implementations in two astrophysical simulation codes, PLUTO and KORAL. We quantitatively compare results obtained between relativistic and non-relativistic, resistive and non-resistive, as well as 2D and 3D setups. The results can be of practical use for computational astrophysicists wanting to select the most appropriate numerical codes and modules in astrophysical simulations.
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