Magnetic Flux Transport and the Long-Term Evolution of Solar Active Regions

TL;DR

This study tracks the long-term evolution of solar active regions using He II 304 Å imaging, inferring magnetic flux changes and validating flux transport models, providing insights into solar magnetic activity.

Contribution

It introduces a method to analyze active region evolution using 304 Å images and employs a flux transport model to predict magnetic flux decay.

Findings

Active regions follow a standard emergence and decay pattern.

The flux-luminosity relationship allows magnetic flux inference from 304 Å images.

The AFT model predicts magnetic flux decay accurately with initial conditions.

Abstract

With multiple vantage points around the Sun, STEREO and SDO imaging observations provide a unique opportunity to view the solar surface continuously. We use He II 304 A data from these observatories to isolate and track ten active regions and study their long-term evolution. We find that active regions typically follow a standard pattern of emergence over several days followed by a slower decay that is proportional in time to the peak intensity in the region. Since STEREO does not make direct observations of the magnetic field, we employ a flux-luminosity relationship to infer the total unsigned magnetic flux evolution. To investigate this magnetic flux decay over several rotations we use a surface flux transport model, the Advective Flux Transport (AFT) model, that simulates convective flows using a time-varying velocity field and find that the model provides realistic predictions when information about the active region's magnetic field strength and distribution at peak flux is available. Finally, we illustrate how 304 \AA\ images can be used as a proxy for magnetic flux measurements when magnetic field data is not accessible.