Spatial distribution of jets in solar active regions

TL;DR

This study investigates the spatial distribution of coronal jets in solar active regions, revealing they predominantly occur at edges and around strong sunspots, with jet frequency increasing with active region age.

Contribution

It introduces a methodology for determining jet positions and lengths, and provides new insights into the preferred locations and dependence on active region age.

Findings

Jets are more frequent at active region edges.

Older active regions produce more jets.

Jets are mainly located around strong sunspots.

Abstract

Context. Solar active regions are known to have jets. These jets are associated with heating and the release of particles into the solar wind. Aim. Our aim is to understand the spatial distribution of coronal jets within active regions to understand if there is a preferential location for them to occur. Methods. We analysed five active regions using Solar Dynamics Observatory Atmospheric Imaging Assembly data over a period of 2-3.5 days when the active regions were close to disk centre. Each active region had a different age, magnetic field strength, and topology. We developed a methodology for determining the position and length of the jets. Results. Jets are observed more frequently at the edges of the active regions and are more densely located around a strong leading sunspot. The number of coronal jets for our active regions is dependent on the age of the active region. The older active regions produce more jets than younger ones. Jets were observed dominantly at the edges of the active regions, and not as frequently in the centre. The number of jets is independent of the average unsigned magnetic field and total flux density in the whole active region. The jets are located around the edges of the strong leading sunspot.