Near-Field Effects of Cherenkov Radiation Induced by Ultra High Energy Cosmic Neutrinos

Abstract

The radio approach for detecting the ultra-high energy cosmic neutrinos has become a mature field. The Cherenkov pulse in radio detection originates from the charge excess of particle showers due to Askaryan effect. The conventional way of calculating the Cherenkov pulse by making far- field approximation fails when the size of elongated showers become comparable with detection distance. We investigate the Cherenkov pulse in near-field by a numerical code based on the finite- difference time-domain (FDTD) method. Our study shows that the near-field radiation exhibits very different behaviors from the far-field one and therefore can be easily recognized. For ground array neutrino detectors, the near-field radiation would provide a unique signature for ultra high energy electromagnetic showers induced by the electron neutrino charge-current interaction. This can be useful in neutrino flavor identification.

14 pages, 13 figures

References in corpus (3)

• High Performance Direct Gravitational N-body Simulations on Graphics Processing Units -- II: An implementation in CUDA
• GAMER: a GPU-Accelerated Adaptive Mesh Refinement Code for Astrophysics
• SAPPORO: A way to turn your graphics cards into a GRAPE-6

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• Askaryan radiation from neutrino-induced showers in ice
• Calculations of electric fields for radio detection of Ultra-High Energy particles
• Complex Analysis of Askaryan Radiation: A Fully Analytic Treatment including the LPM effect and Cascade Form Factor
• Feasibility of Determining Diffuse Ultra-High Energy Cosmic Neutrino Flavor Ratio through ARA Neutrino Observatory
• Prospects of Probing the Radio Emission of Lunar UHECRv Events
• The Strategy of Discrimination between Flavors for Detection of Cosmogenic Neutrinos