  The magnetic field through the magnetic reconnection process affects the
dynamics and structure of astrophysical systems. Numerical simulations are the
tools to study the evolution of these systems. However, the resolution,
dimensions, resistivity, and turbulence of the system are some important
parameters to take into account in the simulations. In this paper, we
investigate the evolution of magnetic energy in astrophysical simulations by
performing a standard test problem for MHD codes, Orszag-Tang. We estimate the
numerical dissipation in the simulations using state-of-the-art numerical
simulation code in astrophysics, PLUTO. The estimated numerical resistivity in
2D simulations corresponds to the Lundquist number $\approx 10^{4}$ in the
resolution of $512\times512$ grid cells. It is also shown that the plasmoid
unstable reconnection layer can be resolved with sufficient resolutions. Our
analysis demonstrates that in non-relativistic magnetohydrodynamics
simulations, magnetic and kinetic energies undergo conversion into internal
energy, resulting in plasma heating.
