Authors: Anastasia Kuske (NJIT), Bin Chen (NJIT), Gelu Nita (NJIT)

Type III radio bursts, which are characterized by rapid frequency drifts, are frequently observed solar radio phenomena. They are often associated with the dynamic processes that occur in the solar corona, including the acceleration and propagation of fast electron streams. These bursts typically indicate underlying energetic events, such as solar flares and coronal mass ejections, which contribute to the complex and rapidly changing conditions in the corona. Type III bursts are believed to be generated by streams of fast electrons traveling through the solar corona; they can occur as isolated events or as part of longer-term Type III storms, and are indicative of the highly dynamic processes within the corona.

The Owens Valley Radio Observatory Long Wavelength Array (OVRO-LWA) has observed many instances of these bursts, highlighting the need for robust detection and analysis methods to understand their frequency and distribution over time. By examining the evolution of Type III bursts, from periods of intense activity, also known as solar storms, to times of relative quiet, this research aims to uncover patterns and mechanisms driving these phenomena. The problem of identifying and analyzing Type III bursts lies in the lack of standardized analysis methods, particularly concerning their rapid frequency drifts, which hinder a comprehensive understanding of their properties and long-term evolution. Here we work on developing algorithms that leverage features such as frequency, intensity, and spectral characteristics to enable rapid detection.