Outflows at the Edges of an Active Region in a Coronal Hole: A Signature of Active Region Expansion?

TL;DR

This study uses 3D simulations to show that active region expansion in the solar corona can drive plasma outflows at the edges of active regions, matching many observed characteristics.

Contribution

The paper demonstrates through simulation that active region expansion can accelerate plasma outflows, providing a plausible mechanism alongside reconnection.

Findings

Outflows are accelerated by active region expansion.

Simulated outflows reach velocities up to 45 km/sec.

Characteristics of simulated outflows match observations.

Abstract

Outflows of plasma at the edges of active regions surrounded by quiet Sun are now a common observation with the Hinode satellite. While there is observational evidence to suggest that the outflows are originating in the magnetic field surrounding the active regions, there is no conclusive evidence that reveals how they are driven. Motivated by observations of outflows at the periphery of a mature active region embedded in a coronal hole, we have used a three-dimensional simulation to emulate the active region's development in order to investigate the origin and driver of these outflows. We find outflows are accelerated from a site in the coronal hole magnetic field immediately surrounding the active region and are channelled along the coronal hole field as they rise through the atmosphere. The plasma is accelerated simply as a result of the active region expanding horizontally as it develops. Many of the characteristics of the outflows generated in the simulation are consistent with those of observed outflows: velocities up to 45 km per sec, properties akin to the coronal hole, proximity to the active region's draining loops, expansion with height, and projection over monopolar photospheric magnetic concentrations. Although the horizontal expansion occurs as a consequence of the active region's development in the simulation, expansion is also a general feature of established active regions. Hence, it is entirely possible and plausible that the expansion acceleration mechanism displayed in the simulation is occurring in active regions on the Sun and, in addition to reconnection, is driving the outflows observed at their edges.