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Cosmic rays are messengers from highly energetic events in the Universe.These rare ultra-high-energy particles can be detected efficiently and in anaffordable way using large arrays of radio antennas. Linearly polarizedgeomagnetic emission is the dominant emission mechanism produced when chargedparticles in air showers get deflected in the Earth's magnetic field. Thesub-dominant Askaryan emission is radially polarized and produced due to thetime-varying negative-charge excess in the shower front. The relative amplitudeof these two emission components depends on various air shower parameters, suchas the arrival direction and the depth of the shower maximum. We studied thesedependencies using CoREAS simulations of the radio emission from air showers atthe South Pole using a star-shaped antenna layout. On the one hand, theparametrization of the Askaryan-to-geomagnetic ratio can be used as input for amore accurate reconstruction of the shower energy. On the other hand, ifmeasured precisely enough, this ratio may provide a new method to reconstructthe atmospheric depth of the shower maximum.

proceedings of 37th international cosmic ray conference — pos(icrc2021)

Parametrization of the Relative Amplitude of Geomagnetic and Askaryan  Radio Emission from Cosmic-Ray Air Showers using CORSIKA/CoREAS Simulations  (ICRC2021)