Self-Organization of Reconnecting Plasmas to Marginal Collisionality in the Solar Corona

TL;DR

This paper investigates how coronal loops in the solar corona self-organize to a state of marginal collisionality through magnetic reconnection, using hydrodynamic simulations to reveal stable and cyclic behaviors influenced by heating rates and plasma density.

Contribution

It introduces a model demonstrating that coronal loops naturally regulate their density and heating to maintain marginal collisionality, supported by numerical simulations showing stable and cyclic regimes.

Findings

Loops reach a marginally collisionless density state.

Two regimes: stable equilibrium and cyclic heating-cooling.

Density regulation is driven by gravity and heating dependence.

Abstract

We explore the suggestions by Uzdensky (2007) and Cassak et al. (2008) that coronal loops heated by magnetic reconnection should self-organize to a state of marginal collisionality. We discuss their model of coronal loop dynamics with a one-dimensional hydrodynamic calculation. We assume that many current sheets are present, with a distribution of thicknesses, but that only current sheets thinner than the ion skin depth can rapidly reconnect. This assumption naturally causes a density dependent heating rate which is actively regulated by the plasma. We report 9 numerical simulation results of coronal loop hydrodynamics in which the absolute values of the heating rates are different but their density dependences are the same. We find two regimes of behavior, depending on the amplitude of the heating rate. In the case that the amplitude of heating is below a threshold value, the loop is in stable equilibrium. Typically the upper and less dense part of coronal loop is collisionlessly heated and conductively cooled. When the amplitude of heating is above the threshold, the conductive flux to the lower atmosphere required to balance collisionless heating drives an evaporative flow which quenches fast reconnection, ultimately cooling and draining the loop until the cycle begins again. The key elements of this cycle are gravity and the density dependence of the heating function. Some additional factors are present, including pressure driven flows from the loop top, which carry a large enthalpy flux and play an important role in reducing the density. We find that on average the density of the system is close to the marginally collisionless value.