| Summary: | 碩士 === 國立臺灣大學 === 物理研究所 === 100 === Askaryan Radio Array (ARA) is an observatory designed to detect the radio frequency (RF) Cherenkov radiation generated by the shower induced by ultra high energy (UHE) cosmic neutrino whose energy lies between 10^17eV and 10^21eV. Tracing the UHE neutrinos is the best way to know the origin and the evolution of the cosmic accelerators, because neutrinos are undeflected by magnetic fields and unhindered by interactions with cosmic microwave background (CMB) when it traverses the universe from the source. ARA Observatory, to be located at the South Pole in Antarctica, takes abundant ice as the target. When UHE neutrinos propagate through the ice, they interact with the nucleons in the ice and generate the Cherenkov radiation via the Askaryan effect. In order to reconstruct more precisely the incident directions of the UHE neutrinos so as to identify their sources, it is desirable to explore different design geometries of the ARA array. We find the optimized configuration of ARA Observatory consists of 49 stations located on a hexagonal lattice with 12 antennas per station. The station spacing is 3 km, string spacing and antenna spacing is 30 m. It means the adjacent antenna spacing is 10 m which is the shortest distance in our simulation. There are three Vpol antennas and one Hpol antenna in a string with the sequence is Vpol-Vpol-Hpol-Vpol.
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