Type IV Radio Bursts and Associated Active Regions in the Sunspot Cycle 24

TL;DR

This study analyzes the spatial distribution of Type IV solar radio bursts and their active regions during solar cycle 24, revealing patterns related to burst types and their potential for understanding coronal mass ejections.

Contribution

It categorizes active regions associated with Type IV bursts based on their solar disk location and examines their relation to CMEs, providing insights into their physical properties.

Findings

Most stationary Type IV bursts are near disk center (60-70%).

Moving Type IV bursts are more evenly distributed across the solar surface.

Active regions near disk center are useful for studying CME properties.

Abstract

In this article, the association of solar radio type IV bursts with active region location on the Sun is studied for the solar cycle 24. The active regions associated with moving and stationary type IV bursts are categorised as close to disk center and far from disk center regions based on their location on the solar surface (i.e, $\leq 45^{\circ}$ or $\geq 45^{\circ}$, respectively). The location of the active regions associated with type IV bursts accompanied with coronal mass ejections (CMEs) are also studied. We found that $\approx 30-40 \%$ of the active regions are located far from disk center for all the bursts. It is found that most of the active regions associated with stationary type IV bursts are close to disk center ($\approx 60-70 \%$). The active regions associated with moving type IV bursts are more evenly distributed across the surface, i.e $\approx 56 \%$ and $\approx 44 \%$, close to disk center and far from disk center regions, respectively. Most of the burst having active region close to disk center indicate that these bursts can be used to obtain physical properties such as electron density and magnetic fields of the coronal mass ejections responsible for geomagnetic storms.