![]() The array is located at Sharjah Academy for Astronomy, Space Sciences and Technology (SAASST) at 25☁7' 09.6'' N, 55° 27' 48.1'' E, in Sharjah, UAE.Ī log-periodic dipole antenna (LPDA) is a very important tool for radio observations of the sun. A test was performed to show the response of the array to artificially generated signals. The array showed variant levels of radio noise of different combined stages of the array. ![]() IFF UPDATE MY BACKGROUND TO NASA PICTURE OF THE DAY PROThe results of the simulations were further used to generate the beam patterns of the prototype and the array using Radio-Jupiter Pro Software. Thetotalgainofthearrayisfoundtobe12.36dBi. Simulation results of antenna beam width for the array, performed using EZNEC Antenna Software, are included. The receiver of the telescope is designed to operate at 20.1MHz to conduct observations of specific celestial activities such as Jupiter-Io interactions, solar bursts, and the background radio emission of the Milky Way. The main aim is to construct a system to initiate undergraduate students to radio astronomy research. This paper discusses the process of constructing a decametric radio telescope array, the first of its kind in the Gulf Cooperation Council area, using 4 dual-dipole antenna units. It was also recorded that the coronal mass ejection followed this solar flare event with the speed of nearly 2000 km/s and directed toward the Earth which then produced intense geomagnetic storm on the Earth the next day. The frequency drift rate for the solar burst was 2.15 MHz/s which proved that this type III is a fast drift burst. The active region 486 alone had a sunspot number of 74 which is quite high, hence it produced a flare with the solar wind speed of 800 km/s and a solar radio burst type III with the storm type. ![]() The study of the solar flare event was done by observing the sunspot for the past six days to see the changes in the magnetic field of the active region 486 and compared it to the solar radio data for the nature of the solar flares. Another data for this study were collected from the online database of Solar Monitor and Space Weather Live website where they provided the data from NOAA and SDO/AIA publicly. The intense solar flare was detected by the CALLISTO system as the type III solar burst. This active region produced quite a strong solar flare with the X 17 class on 28 th October 2003. This paper focuses on the study of active region (AR) 486 from the 171 Å wavelength in conjunction with solar radio burst data from the e-CALLISTO. ![]()
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