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By Thomas Meures

The target of the venture offered during this ebook is to observe neutrinos created via resonant interactions of ultrahigh strength cosmic rays at the CMB photon box filling the Universe. during this pioneering first research, the writer places ahead a lot of the research framework, together with calibrations of the digital and antenna geometry, in addition to the advance of algorithms for occasion reconstruction and information aid. whereas in basic terms of the 37 stations deliberate for the Askaryan Radio Array have been utilized in this evaluate of 10 months of information, the research was once in a position to exclude neutrino fluxes above 10 PeV with a restrict no longer faraway from the simplest present restrict set by way of the IceCube detector, a consequence which establishes the radio detection method because the direction ahead to reaching the large volumes had to observe those ultrahigh power neutrinos.

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Extra info for Development of a Sub-glacial Radio Telescope for the Detection of GZK Neutrinos

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Assuming such a changing index of refraction, Snell’s law predicts a down-bending of the path of radio waves in the vertical direction. Different measurements, models and implications for the changing index of refraction are described in [6]. 78 below an ice depth of roughly 200 m. There are different models describing the existing measurements. 1) with z = 0 at the ice surface and z < 0 below. Given such a refraction profile, radio waves cannot reach the detector from everywhere in the ice due to the ray-bending effect.

Therefore, their spacing is chosen to maximize the effective volume of the full ARA array while not counting on coincident events. Such coincidences are in any case expected to be rare due to the comparably tight Cherenkov cones of Askaryan emission. 1 The General Detector Setup 39 Fig. 2 Schematic view of an ARA station, with embedded string details. Surface antennas are not shown in this figure at South Pole by the ARA prototype station, referred to as the ARA TestBed. Its setup and performance is described in detail in [2] and first constraints on a neutrino flux from this detector are presented in [3].

1 The General Detector Setup The ARA detector is planned to consist of widely spread antenna clusters that can each operate as autonomous detectors of the Askaryan emission from neutrino-induced cascades. Such clusters are currently deployed in the South Pole ice, next to the IceCube detector [1], as shown in Fig. 1. As explained in Chaps. 2 and 3, GZK neutrinos interact very rarely and need large detector volumes of several cubic kilometers to be efficiently detected. The Askaryan emission from neutrino-induced cascades allows to build such large detectors due to the long attenuation length of radio waves in media like ice and salt, which permits a wide sensor spacing.

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