Abstract
Abstract. This article summarises the results of an analysis of solar radio bursts (SRBs) detected by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) spectrometer hosted by the University of Rwanda. The data analysed were detected during the first year (2014–2015) of the instrument operation. Using quick plots provided by the e-CALLISTO website, a total of 201 intense and well-separated solar radio bursts detected by the CALLISTO station located in Rwanda, are found consisting of 4 type II, 175 type III and 22 type IV radio bursts. It is found that all analysed type II and ∼ 37 % of type III bursts are associated with impulsive solar flares, while the minority (∼ 13 %) of type IV radio bursts are associated with solar flares. Furthermore, all type II radio bursts are associated with coronal mass ejections (CMEs), ∼ 44 % of type III bursts are associated with CMEs, and the majority (∼ 82 %) of type IV bursts were accompanied by CMEs. With aid of the atmospheric imaging assembly (AIA) images on board the Solar Dynamics Observatory (SDO), the location of open magnetic field lines of non-flare-associated type III radio bursts are shown. The same images are used to show the magnetic loops in the solar corona for type IV radio bursts observed in the absence of solar flares and/or CMEs. Findings from this study indicate that analysis of SRBs that are observed from the ground can provide a significant contribution to the early diagnosis of solar transients phenomena, such as solar flares and CMEs, which are major drivers of potential space weather hazards.
Highlights
The solar space weather events like coronal mass ejections (CMEs) and solar flares are usually accompanied by solar radio bursts (SRBs), which can be used for a low-cost realtime space weather monitoring (Lobzin et al, 2009)
The analysis shows that all type II radio bursts are associated with solar flares, and ∼ 37 % of the type III and ∼ 13 %
We found that the remaining non-flare-related type III bursts might have been triggered by small-scale features or weak energy events present in the solar corona according to the literature and with the help of atmospheric imaging assembly (AIA)/Solar Dynamics Observatory (SDO) images in the 171 Å bandpass
Summary
The solar space weather events like coronal mass ejections (CMEs) and solar flares are usually accompanied by solar radio bursts (SRBs), which can be used for a low-cost realtime space weather monitoring (Lobzin et al, 2009). Type II radio bursts are the bright radio emissions often associated with CMEs and characterised by a slow-frequency drift rate (≤ −1 MHz s−1; McLean and Labrum, 1985; Nelson and Melrose, 1985). They are excited by magnetohydrodynamics (MHD) shocks in the solar atmosphere (Nelson and Melrose, 1985; Cliver et al, 1999; Nindos et al, 2008, 2011; Vršnak and Cliver, 2008).
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