Practical and accurate calculations of Askaryan radiation

Álvarez-Muñiz, J.; Romero-Wolf, Andrés; Zas, E.

doi:10.1103/physrevd.84.103003

Cited by 50 publications

(83 citation statements)

References 47 publications

(97 reference statements)

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“…The first data set was obtained with a prototype setup [27] for AERA; the other one with AERA itself [5][6][7] during its commissioningphasewhileit consistedof only24 stations.Inaddition,we will compare these data sets with results from different types of calculations outlined in Refs. [28][29][30][31][32][33][34].…”

Section: Introductionmentioning

confidence: 99%

Probing the radio emission from air showers with polarization measurements

Aab¹,

Abreu²,

Aglietta³

et al. 2014

Phys. Rev. D

114

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The emission of radio waves from air showers has been attributed to the so-called geomagnetic emission process. At frequencies around 50 MHz this process leads to coherent radiation which can be observed with rather simple setups. The direction of the electric field induced by this emission process depends only on the local magnetic field vector and on the incoming direction of the air shower. We report on measurements of the electric field vector where, in addition to this geomagnetic component, another component has been observed that cannot be described by the geomagnetic emission process. The data provide strong evidence\ud hat the other electric field component is polarized radially with respect to he shower axis, in agreement\ud with predictions made by Askaryan who described radio emission from particle showers due to a negative\ud charge excess in the front of the shower. Our results are compared to calculations which include the\ud radiation mechanism induced by this charge-excess proces

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Section: Introductionmentioning

confidence: 99%

Probing the radio emission from air showers with polarization measurements

Aab¹,

Abreu²,

Aglietta³

et al. 2014

Phys. Rev. D

114

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show abstract

“…In addition to the fact that both simulation tools are based on different hadronic and electromagnetic interaction codes to handle particle interaction, they also use different models to calculate the radio emission by the simulated particle showers. The "endpoint" formalism [3][4] applied in CoREAS [5] based on CORSIKA and the "ZHS" formalism [6] applied in ZHAireS [7] based on AIRES. The two formalisms calculate the electric field of the moving charged particles in the shower.…”

Section: Motivationmentioning

confidence: 99%

Modelling of radio emission in the SLAC T-510 Experiment using microscopic Geant4 simulations

Zilles¹,

Bechtol²,

Belov³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The SLAC T-510 experiment was designed to verify established microscopic models for simulation of radio emission from air-showers by reproducing the physics under controlled lab conditions. For this verification, the simulation toolkit Geant4 was expanded by the calculation of the emitted radio signal with the "endpoint" and the "ZHS" formalisms in parallel. We present and compare the results of the two simulation approaches, taking into account the details of the experimental set-up such as the beam energy, target geometry and material, and the magnetic field configuration. We put special emphasis on the discussion of the effects due to refraction and transition radiation and show a comparison of the simulation results with the measured data of the SLAC T-510 Experiment.

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“…Because cosmic-rays with energies above 4×10 19 eV interact with the cosmic microwave background radiation, they have a range limited to ≈ 75 Mpc. These p + γ interactions excite a ∆ + resonance from the proton.…”

Section: Introductionmentioning

confidence: 99%

“…Between this polarization measurement, and the determination of the frequency spectrum, the neutrino arrival direction can be determined, given enough channels above background [15]. Monte Carlo simulations have been used to predict the electric fields that would be produced by the interactions in ice [18,19]. Both charged current (CC) and neutral current (NC) interactions are of interest.…”

Section: Introductionmentioning

confidence: 99%

Future Prospects of UHE Neutrino Detection with Electromagnetic Fields

Hanson¹

2017

Proceedings of the 7th International Workshop on Very High Energy Particle Astronomy in 2014 (VHEPA2014)

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In recent years, the field of ultra-high energy (≥ 1 PeV) neutrino astronomy has begun to develop. Both Cerenkov photon detectors and radio detectors have been constructed, and an extraterrestrial signal has finally been observed near 1 PeV. Both particle physics and astrophysics drive the development of this field. Ultra-high energy (UHE) neutrinos generated by the GZK process could reveal the origin of cosmic rays, by pointing to the source. A sample of neutrino interactions with terrestrial matter at center-of-mass energies ≥10 TeV also presents opportunities to quantify the neutrino cross-section and flavor physics at previously unreachable energies. Finally, astrophysical phenomena with particle energies greater than the electro-weak scale and redshift z ≥ 0.1 will never be observed until the field of UHE neutrino astronomy matures. Thus, Askaryan effect-based radio detectors are becoming increasingly important, and the Antarctic Ross Ice Shelf Antenna Neutrino Array (ARIANNA) is a detector designed in this fashion. The electromagnetic signal in detectors such as ARIANNA will be described, along with various effects that modify it.

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Practical and accurate calculations of Askaryan radiation

Cited by 50 publications

References 47 publications

Probing the radio emission from air showers with polarization measurements

Probing the radio emission from air showers with polarization measurements

Modelling of radio emission in the SLAC T-510 Experiment using microscopic Geant4 simulations

Future Prospects of UHE Neutrino Detection with Electromagnetic Fields

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