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A comparison study of CORSIKA and COSMOS simulations for extensive air showers
Roh, S.,Kim, J.,Ryu, D.,Kang, H.,Kasahara, K.,Kido, E.,Taketa, A. North-Holland ; Elsevier Science Ltd 2013 Astroparticle physics Vol.44 No.-
Cosmic rays with energy exceeding ~10<SUP>18</SUP>eV are referred to as ultra-high energy cosmic rays (UHECRs). Monte Carlo codes for extensive air shower (EAS) simulate the development of EASs initiated by UHECRs in the Earth's atmosphere. Experiments to detect UHECRs utilize EAS simulations to estimate their energy, arrival direction, and composition. In this paper, we compare EAS simulations with two different codes, CORSIKA and COSMOS, presenting quantities including the longitudinal distribution of particles, depth of shower maximum, kinetic energy distribution of particle at the ground, and energy deposited to the air. We then discuss implications of our results to UHECR experiments.
Dependency of the Plasma Loading Resistance on the RF Power for KSTAR ICRF Heating
S. J. Wang,김선호,J. G. Kwak,S. K. Kim,H. Kasahara,T. Seki,T. Mutoh 한국물리학회 2010 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.57 No.5
The ion cyclotron range of frequency (ICRF) experiment on the KSTAR tokamak is performed without the interference of ion cyclotron resonances so that only electrons are heated component. Maximum 150% local Te increase is measured by the ECE with PRF ∼ 300 kW of f = 44.2 MHz RF pulse with wide range of plasma parameters. The averaged RL deduced from the ICRF pulses during this campaign shows that RL has an increasing trend as PRF increases in the range of PRF = 70 ∼ 280 kW. If the local electron density, ne, around an antenna is added by Δne due to the near-field ionization of the outgassed neutral particles, fast wave propagation will be enhanced by a modified fast wave cutoff layer. This enhancement can be represented by RL showing its linearity as a function of n1/2 e = (n'e +Δne)1/2. The experimental result of a monotonic increase in RL with PRF will give a qualitative base to support recent activities to achieve a high-power-density ITER ICRF antenna by actively increasing RL with additional gas puffing in the vicinity of the antenna.