Flows and magnetic field structures in reconnection regions of simulations of the solar atmosphere: do flux pile-up models work?

TL;DR

This paper investigates magnetic reconnection in solar atmosphere simulations, confirming flux pile-up models and standard reconnection mechanisms through high-resolution MHD simulations of the photosphere and chromosphere.

Contribution

It demonstrates that flux pile-up models accurately describe magnetic reconnection structures in solar atmosphere simulations, supported by high-resolution data.

Findings

Magnetic reconnection consistent with flux pile-up models observed.

Standard Sweet-Parker reconnection identified in stronger magnetic fields.

Flow and magnetic structures align with theoretical predictions.

Abstract

We study the process of magnetic field annihilation and reconnection in simulations of magnetised solar photosphere and chromosphere with magnetic fields of opposite polarities and constant numerical resistivity. Exact analytical solutions for reconnective annihilations are used to interpret the features of magnetic reconnection in simulations of flux cancellation in the solar atmosphere. We use MURaM high-resolution photospheric radiative magneto-convection simulations to demonstrate the presence of magnetic field reconnection consistent with the magnetic flux pile-up models. Also, a simulated data-driven chromospheric magneto-hydrodynamic simulation is used to demonstrate magnetic field and flow structures, which are similar to the ones theoretically predicted. Both simulations demonstrate flow and magnetic field structures roughly consistent with accelerated reconnection with magnetic flux pile-up. The presence of standard Sweet-Parker type reconnection is also demonstrated in stronger photospheric magnetic fields.