Thunderstorm observations by air-shower radio antenna arrays

Apel, W. D.; Arteaga, J.C.; Bähren, L.; Bekk, K.; Bertaina, M.; Biermann, P. L.; Blümer, J.; Bozdog, H.; Brâncuş, I.M.; Buchholz, P.; Buitink, S.; Cantoni, E.; Чиавасса, А.; Daumiller, K.; Souza, V. de; Pierro, F. Di; Döll, P.; Ender, Moses; Engel, R.; Falcke, H.; Finger, M.; Fuhrmann, D.; Gemmeke, H.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Horneffer, A.; Huber, Daniel; Huege, T.; Isar, P. G.; Kampert, K.‐H.; Kang, D.; Krömer, O.; Kuijpers, J.; Link, K.; Łuczak, P.; Ludwig, M.; Melissas, M.; Morello, C.; Nehls, S.; Oehlschläger, J.; Palmieri, N.; Pierog, T.; Rautenberg, J.; Rebel, H.; Roth, M.; Rühle, C.; Sǎftoiu, A.; Schieler, H.; Schmidt, A.; Schröder, Frank G.; Sima, O.; Toma, G.; Trinchero, G.; Weindl, A.; Wochele, J.; Wommer, M.; Zabierowski, J.; Zensus, J. A.

doi:10.1016/j.asr.2011.06.003

Cited by 23 publications

(21 citation statements)

References 16 publications

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“…Since only the relativistic airshower electrons and positrons have a significant effect on the simulated radio emission [62], other particles are neglected. Moreover, acceleration by electric fields is neglected, since experimental results indicate that atmospheric electric fields do not have any significant effect on the radio emission during normal weather conditions [43,44]. Finally, REAS 3.11 and CoREAS both consider a realistic, height-dependent refractive index of the atmosphere, which changes the coherence conditions for any radio emission generated by the air shower.…”

Section: Simulationsmentioning

confidence: 99%

“…The signal-to-noise ratio is calculated as the height of a Gaussian fit to the CC beam smoothed by block-averaging, divided by the RMS of the smoothed CC beam in a part of the trace before the radio pulse. Furthermore, we exclude events for which we measured a high atmospheric electrical field at ground (E atm > 3000 V/m), since this can significantly affect the radio emission of air showers [43,44].…”

Section: Event Selectionmentioning

confidence: 99%

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Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Apel

Arteaga‐Velázquez

Bähren

et al. 2013

Astroparticle Physics

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Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations AbstractCosmic ray air showers emit radio pulses at MHz frequencies, which can be measured with radio antenna arrays -like LOPES at the Karlsruhe Institute of Technology in Germany. To improve the understanding of the radio emission, we test theoretical descriptions with measured data. The observables used for these tests are the absolute amplitude of the radio signal, and the shape of the radio lateral distribution. We compare lateral distributions of more than 500 LOPES events with two recent and public Monte Carlo simulation codes, REAS 3.11 and CoREAS (v 1.0). The absolute radio amplitudes predicted by REAS 3.11 are in good agreement with the LOPES measurements. The amplitudes predicted by CoREAS are lower by a factor of two, and marginally compatible with the LOPES measurements within the systematic scale uncertainties. In contrast to any previous versions of REAS, REAS 3.11 and CoREAS now reproduce the shape of the measured lateral distributions correctly. This reflects a remarkable progress compared to the situation a few years ago, and it seems that the main processes for the radio emission of air showers are now understood: The emission is mainly due to the geomagnetic deflection of the electrons and positrons in the shower. Less important but not negligible is the Askaryan effect (net charge variation). Moreover, we confirm that the refractive index of the air plays an important role, since it changes the coherence conditions for the emission: Only the new simulations including the refractive index can reproduce rising lateral distributions which we observe in a few LOPES events. Finally, we show that the lateral distribution is sensitive to the energy and the mass of the primary cosmic ray particles.

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Section: Simulationsmentioning

confidence: 99%

Section: Event Selectionmentioning

confidence: 99%

Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Apel

Arteaga‐Velázquez

Bähren

et al. 2013

Astroparticle Physics

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“…By ionizing the traversed air, the shower front builds up a time-varying net charge excess causing radially polarized radio emission, also called Askaryan emission. Not shown: In thunderstorm clouds particle acceleration by electric fields is a third mechanism [8,9] (adapted from [1]).…”

Section: Basic Properties Of the Radio Signalmentioning

confidence: 99%

Air Shower Detection by Arrays of Radio Antennas

Schröder

2019

EPJ Web Conf.

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Antenna arrays are beginning to make important contributions to high energy astroparticle physics supported by recent progress in the radio technique for air showers. This article provides an update to my more extensive review published in Prog. Part. Nucl. Phys. 93 (2017) 1. It focuses on current and planned radio arrays for atmospheric particle cascades, and briefly references to a number of evolving prototype experiments in other media, such as ice. While becoming a standard technique for cosmic-ray nuclei today, in future radio detection may drive the field for all type of primary messengers at PeV and EeV energies, including photons and neutrinos. In cosmic-ray physics accuracy becomes increasingly important in addition to high statistics.Various antenna arrays have demonstrated that they can compete in accuracy for the arrival direction, energy and position of the shower maximum with traditional techniques. The combination of antennas and particles detectors in one array is a straight forward way to push the total accuracy for high-energy cosmic rays for low additional cost. In particular the combination of radio and muon detectors will not only enhance the accuracy for the cosmic-ray mass composition, but also increase the gamma-hadron separation and facilitate the search for PeV and EeV photons. Finally, the radio technique can be scaled to large areas providing the huge apertures needed for ultra-high-energy neutrino astronomy. CoREAS simulationsfor South Pole (IceTop site): 10 PeV proton at 61° zenith

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“…Probing atmospheric electric fields during thunderstorms Radio detection of air showers is also used for auxiliary science, such as the measurements of electric fields in the atmosphere during thunderstorms [31,32,23]. The footprint of the radio emission from an air shower, which developed during a thunderstorm is shown in Fig.…”

Section: Confirmation Of Simulation Codesmentioning

confidence: 99%

“…, ⇤ = 0, = 0) is the electromagnetic field ined from the manufacturer [32]. H(⇥) corthe source antenna is linearly polarized, only ⇥) 2 is proportional to power, so that X(⇥) is s of 65400 samples of 5 ns, corresponding MHz range.…”

Section: Pos(icrc2015)033mentioning

confidence: 99%

Radio detection of Cosmic Rays with LOFAR

Hörandel¹

2016

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

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When high-energy cosmic rays (ionized atomic nuclei) impinge on the atmosphere of the Earth they interact with atomic nuclei and initiate cascades of secondary particles -the extensive air showers. Many of the secondary particles in the air showers are electrons and positrons. They cause radiation in the frequency range of tens of MHz. The LOFAR radio telescope detects this radiation in the frequency range 30 to 240 MHz. LOFAR has a high antenna density and good time resolution. In turn, the properties of the radio emission are measured in detail. The properties of the shower-inducing cosmic rays are derived from the air shower measurements, namely their direction, energy, and particle type (atomic mass). The uncertainties achieved are competative to established techniques. This demonstrates that the radio technique is now a standard tool to measure extensive air showers and to study the properties of the incoming cosmic rays. The mean logarithmic mass of cosmic rays as measured with LOFAR is derived as a function of energy. In an examplary study, these data are used to show that the radio measurements of air showers are now in a state to discriminate astrophysical models of the origin of cosmic rays. PoS(ICRC2015)033Radio Detection of Cosmic Rays with LOFAR J.R. Hörandel thus the amount of observing time in a given frequency band is not controlled by the cosmic ray project. In parallel to any observation the tile-beamformed data from all tiles are filled into ring buffers (Transient Buffer Boards), from which the last 5 s of data can be recorded when triggered. Triggers can be generated by inspecting the data with an on-board FPGA 1 or received through the LOFAR control software. In order to record cosmic-ray pulses, the dense core of LOFAR is equipped with an array of particle detectors [20], as also shown in Fig. 2. In routine observations, coincidences of several particle detectors trigger a read-out of the ring buffers [18].The HBAs can be sampled at two different clock frequencies, which allows for several different observing bands. The one mostly used in the present data-set is an event. During processing, the signals from all tiles in a station are first coherently beamformed in the cosmic-ray arrival direction as reconstructed from the particle data. When a significant signal, with a signal-to-noise ratio exceeding three in amplitude, is detected in the beamformed signal the station is selected for further processing and the event is selected as a cosmic ray candidate. Using a smaller search window, around the peak in the beamformed signal, a pulse search is then performed on the Hilbert envelope of the up-sampled signals from each tile. Up-sampling, by a factor 16, is needed such that the pulse maximum search is not the limiting factor in achieving the required time resolution. From the arrival times of those pulse maxima for which the signal-to-noise ratio in amplitude exceeds three, the direction of the cosmic ray is reconstructed. Additionally the amplitude (in each instrumental polarization) and...

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Thunderstorm observations by air-shower radio antenna arrays

Cited by 23 publications

References 16 publications

Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Air Shower Detection by Arrays of Radio Antennas

Radio detection of Cosmic Rays with LOFAR

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