A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating

TL;DR

This paper explores a new model for solar atmospheric heating based on magnetic flux cancellation and 3D reconnection, motivated by recent high-resolution observations.

Contribution

It introduces a flux cancellation-driven reconnection model as an alternative to traditional braiding models for solar heating.

Findings

Flux cancellation can produce significant energy release at various heights.

The energy release depends on flux size, cancellation speed, and magnetic field strength.

The model aligns with recent high-resolution observations of the solar atmosphere.

Abstract

Nanoflare models for heating the solar corona usually assume magnetic braiding and reconnection as the source of the energy. However, recent observations at record spatial resolution from the {\sc Sunrise} balloon mission suggest that photospheric magnetic flux cancellation is much more common than previously realised. We therefore examine the possibility of three-dimensional reconnection driven by flux cancellation as a cause of chromospheric and coronal heating. In particular, we estimate how the heights and amount of energy release produced by flux cancellation depend on flux size, flux cancellation speed and overlying field strength.