Design strategies for antenna array to monitor the sun in low-frequency range

Abstract

Radio signal wavelengths typically range from centimeters to meters, so the waves themselves are not nanometers. The connection to the nanoscale lies in the materials and manufacturing processes within the telescope system, the design of antenna arrays and their orientation toward the observed object are among the most important considerations in communications systems and the construction of modern radio telescopes, particularly low-frequency telescopes. This paper addresses a fundamental methodology for optimizing the design and placement of antenna arrays to enhance performance metrics, including key design considerations in terms of element spacing, array geometry, and feed network structure. Advanced techniques, such as adaptive beamforming and digital signal processing, are being investigated to improve the signal-to-noise ratio and mitigate interference. Several common geometries are used in antenna array design, each with its advantages and characteristics depending on the application. A special array system is used to monitor the sun on top of the Astronomy and Space Department building at the College of Science at the University of Baghdad, which is the subject of our research. This system is a linear array, with antennas arranged in a straight line. This type of antenna is the most common in astronomical studies. A dipole antenna with a length of λ/2 is designed, and two antennas are made with the same specifications in terms of wire length and material to receive the same signal at the same frequency. The system determines the position of the sun based on time and date, tracking the sun throughout the year without moving the antenna. The phase shift angle is calculated, and from there, different wire lengths are made to obtain different resistances compatible with the phase shift angle. The results underscore the need for a tailored approach to antenna array design to maximize the observation of most astronomical phenomena originating from the sun, particularly at low frequencies. This marks the first astronomical system designed for this type of observation.