A flux-independent increase in outflows prior to the emergence of active regions on the Sun

TL;DR

This study reveals a flux-independent increase in outflows prior to active region emergence on the Sun, supported by observations and simulations, suggesting a potential precursor signal for solar activity.

Contribution

It demonstrates a flux-independent outflow increase before active region emergence and links observations with simulations to explore underlying mechanisms.

Findings

Flow divergence increases prior to emergence regardless of flux amount.

Active regions show a remaining converging flow 0.5-1 days before emergence.

Simulations qualitatively support observational results.

Abstract

Emerging active regions are associated with convective flows on the spatial scale and lifetimes of supergranules. To understand how these flows are involved in the formation of active regions, we aim to identify where active regions emerge in the supergranulation flow pattern. We computed supergranulation scale flow maps at the surface for all active regions in the Solar Dynamics Observatory Helioseismic Emerging Active Region Survey. We classified each of the active regions into four bins, based on the amplitude of their average surface flow divergence at emergence. We then averaged the flow divergence over the active regions in each bin as a function of time. We also considered a corresponding set of control regions. We found that, on average, the flow divergence increases during the day prior to emergence at a rate independent of the amount of flux that emerges. By subtracting the averaged flow divergence of the control regions, we found that active region emergence is associated with a remaining converging flow at 0.5-1 days prior to emergence. This remnant flow, $\Delta \, \mathrm{div} \, \mathbf{v_h} = (-4.9 \pm 1.7) \times 10^{-6}$ 1/s, corresponds to a flow speed of 10-20 m/s (an order of magnitude less than supergranulation flows) out to a radius of about 10 Mm. We show that these observational results are qualitatively supported by simulations of a small bipole emerging through the near-surface convective layers of the Sun. The question remains whether these flows are driving the emergence, or are caused by the emergence.