Solar radio activities using spectrometer and heliograph / Mohd Shazwan Mohd Radzi

Mohd Shazwan , Mohd Radzi (2024) Solar radio activities using spectrometer and heliograph / Mohd Shazwan Mohd Radzi. Masters thesis, Universiti Malaya.

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Abstract

Compound Astronomical Low frequency Low cost Instrument for Spectroscopy and Transportable Observatory (CALLISTO) is one of the instruments used to detect solar radio bursts at 45 MHz to 870 MHz which mainly used in this work. The novelty of this work is that the relationship between the occurrence of solar radio bursts and solar flares was investigated by considering the time interval between them. The associated solar flare class was also considered since all solar radio bursts in this study were associated with solar flares. In addition, each type of solar radio burst has been divided into two groups depending on whether their magnetic field lines topology are open or closed. The classification mainly depending on the existence of shock wave based on wave speed calculated for each type of burst. Based on the wave speed obtained, it concluded that type I, III, and V having an open magnetic field line topology with the associated flares differed between the M, C, and X classes. While for type II and IV declared to have closed magnetic field line topology with M and C class associated flare. Moreover, the results of this study was conformed that RDF has a linear relationship with solar radio burst detection and RDF frequency fits through the plots and linear line of the CALLISTO detections. This study also shows the relationship between solar activity and earthquake activity, with a total of 141 events recorded. In this statistical analysis, the distribution of the SWD plot with earthquake magnitude obtained was fair enough to indicate relationship between solar activity and earthquakes. In this study also, the emission mechanism is determined separately for the types II and III SRB while always taking into account the specific characteristics of each type. The maximum brightness temperature and degree of polarization for the Type II solar radio burst obtained were varied between 107 K and 1010 K and 3% and 27%, respectively. While for type III burst, brightness temperature and degree of polarization were varied between 108 K and 109 K and 7% and 9%, respectively. Based on these characteristics, this study suggests this type II burst was originated from Electron Cyclotron Maser (ECM) emission while type III originated from Gyrosynchrotron emission. As the preliminary for future work, one general network transmission test was done as the requirement for E-VLBI which a technique that involved interferometry to enhance the resolution of signals received. The network test has shown reasonable results with 812 Mbps (Client) and 618 Mbps (Server) of transfer rate for Universiti Malaya (UM) station while 19.5 Mbps (Client) and 18.9 Mbps (Server) for Jelebu station (JEL). Subsequently, a data transmission test also was conducted between Universiti Malaya (UM) and Yunnan Astronomical Observatory (YNAO) to develop this interferometry technique for future solar radio observations. The results obtained were barely satisfactory with 2.1 Mbps for downloading and 1.6 Mbps for uploading processes with no packet loss detected. As conclusion, an interferometry procedure with real-time data transmission should be implemented in every solar radio observation to improve the quality of the data and the generated images.

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