Type IV Radio Bursts and Associated Active Regions in the Sunspot Cycle 24
arXiv:2205.02482 · doi:10.1007/s11207-022-02032-2
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, or , respectively). The location of the active regions associated with type IV bursts accompanied with coronal mass ejections (CMEs) are also studied. We found that 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 (). The active regions associated with moving type IV bursts are more evenly distributed across the surface, i.e and , 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.
3 figures, 1 table, Accepted for publication in Solar Physics
References in corpus (7)
- Estimation of a Coronal Mass Ejection Magnetic Field Strength using Radio Observations of Gyrosynchrotron Radiation
- An estimate of the magnetic field strength associated with a solar coronal mass ejection from low frequency radio observations
- Variable emission mechanism of a Type IV radio burst
- Strength of the Solar Coronal Magnetic field - A Comparison of Independent Estimates Using Contemporaneous Radio and White-light Observations
- CME liftoff with high-frequency fragmented type II burst emission
- Moving solar radio bursts and their association with coronal mass ejections
- On the occurrence of type IV solar radio bursts in the solar cycle 24 and their association with coronal mass ejections