Evolution of the Magnetic Field Distribution of Active Regions

TL;DR

This study investigates how the magnetic field distribution in active regions evolves over time, revealing that flux dispersal involves complex processes beyond classical diffusion, likely influenced by convective cells.

Contribution

It introduces a novel analysis of magnetic field distribution slopes over time, challenging classical diffusion models and highlighting the role of convective reprocessing.

Findings

Magnetic field distribution slopes become less steep during emergence and reach a maximum before decay.

Observed slopes differ from classical diffusion predictions, indicating additional flux dispersal mechanisms.

Steep slopes during decay suggest magnetic flux reprocessing by convective cells.

Abstract

Aims. Although the temporal evolution of active regions (ARs) is relatively well understood, the processes involved continue to be the subject of investigation. We study how the magnetic field of a series of ARs evolves with time to better characterise how ARs emerge and disperse. Methods. We examine the temporal variation in the magnetic field distribution of 37 emerging ARs. A kernel density estimation plot of the field distribution was created on a log-log scale for each AR at each time step. We found that the central portion of the distribution is typically linear and its slope was used to characterise the evolution of the magnetic field. Results. The slopes were seen to evolve with time, becoming less steep as the fragmented emerging flux coalesces. The slopes reached a maximum value of ~ -1.5 just before the time of maximum flux before becoming steeper during the decay phase towards the quiet Sun value of ~ -3. This behaviour differs significantly from a classical diffusion model, which produces a slope of -1. These results suggest that simple classical diffusion is not responsible for the observed changes in field distribution, but that other processes play a significant role in flux dispersion. Conclusions. We propose that the steep negative slope seen during the late decay phase is due to magnetic flux reprocessing by (super)granular convective cells.