The wavelength variation of the granule/intergranule contrast

Bray, R. J.

doi:10.1007/bf00156113

Cited by 9 publications

(18 citation statements)

References 6 publications

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“…So far no neutrino or cosmic-ray events were detected by any of these experiments. Given their sensitivity this is consistent with expectations from traditional air-shower arrays and has been used to set limits for the neutrino and cosmic-ray flux at ZeV energies [3].…”

Section: Radio Observation Of the Moonsupporting

confidence: 69%

Radio detection of cosmic-ray air showers and high-energy neutrinos

Schröder

2017

Progress in Particle and Nuclear Physics

171

145

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In the last fifteen years radio detection made it back to the list of promising techniques for extensive air showers, firstly, due to the installation and successful operation of digital radio experiments and, secondly, due to the quantitative understanding of the radio emission from atmospheric particle cascades. The radio technique has an energy threshold of about 100 PeV, which coincides with the energy at which a transition from the highest-energy galactic sources to the even more energetic extragalactic cosmic rays is assumed. Thus, radio detectors are particularly useful to study the highest-energy galactic particles and ultra-high-energy extragalactic particles of all types. Recent measurements by various antenna arrays like LOPES, CODALEMA, AERA, LOFAR, Tunka-Rex, and others have shown that radio measurements can compete in precision with other established techniques, in particular for the arrival direction, the energy, and the position of the shower maximum, which is one of the best estimators for the composition of the primary cosmic rays. The scientific potential of the radio technique seems to be maximum in combination with particle detectors, because this combination of complementary detectors can significantly increase the total accuracy for air-shower measurements. This increase in accuracy is crucial for a better separation of different primary particles, like gamma-ray photons, neutrinos, or different types of nuclei, because showers initiated by these particles differ in average depth of the shower maximum and in the ratio between the amplitude of the radio signal and the number of muons. In addition to air-shower measurements, the radio technique can be used to measure particle cascades in dense media, which is a promising technique for detection of ultra-high-energy neutrinos. Several pioneering experiments like ARA, ARIANNA, and ANITA are currently searching for the radio emission by neutrino-induced particle cascades in ice. In the next years these two sub-fields of radio detection of cascades in air and in dense media will likely merge, because several future projects aim at the simultaneous detection of both, high-energy cosmic-rays and neutrinos. SKA will search for neutrino and cosmic-ray initiated cascades in the lunar regolith and simultaneously provide unprecedented detail for air-shower measurements. Moreover, detectors with huge exposure like GRAND, SWORD or EVA are being considered to study the highest energy cosmic rays and neutrinos. This review provides an introduction to the physics of radio emission by particle cascades, an overview on the various experiments and their instrumental properties, and a summary of methods for reconstructing the most important air-shower properties from radio measurements. Finally, potential applications of the radio technique in high-energy astroparticle physics are discussed.

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Section: Radio Observation Of the Moonsupporting

confidence: 69%

Radio detection of cosmic-ray air showers and high-energy neutrinos

Schröder

2017

Progress in Particle and Nuclear Physics

171

145

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“…CODALEMA [59], TREND [33], AERA [60], and ARIANNA [38] have shown that autonomous radio detection is feasible, but there remain some open questions: it has to be shown that the trigger can be pure and efficient enough for inclined showers, and there are technical challenges regarding infrastructure, data communication, and reliability of long-term and large-scale remote operation. Alternative ways to large apertures might be provided by observing air-showers with antennas in space [61], or by using the moon as a target [62]. However, these methods require successful proof-of-principle demonstrations, and it is not yet clear how they will compare in terms of measurement accuracy to ground-based antenna arrays.…”

Section: Applications Of the Radio Technique For Air Showersmentioning

confidence: 99%

Status of air-shower measurements with sparse radio arrays

Schröder

2017

EPJ Web Conf.

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Abstract. This proceeding gives a summary of the current status and open questions of the radio technique for cosmic-ray air showers, assuming that the reader is already familiar with the principles. It includes recent results of selected experiments not present at this conference, e.g., LOPES and TREND. Current radio arrays like AERA or Tunka-Rex have demonstrated that areas of several km 2 can be instrumented for reasonable costs with antenna spacings of the order of 200 m. For the energy of the primary particle such sparse antenna arrays can already compete in absolute accuracy with other precise techniques, like the detection of air-fluorescence or air-Cherenkov light. With further improvements in the antenna calibration, the radio detection might become even more accurate. For the atmospheric depth of the shower maximum, X max , currently only the dense array LOFAR features a precision similar to the fluorescence technique, but analysis methods for the radio measurement of X max are still under development. Moreover, the combination of radio and muon measurements is expected to increase the accuracy of the mass composition, and this around-the-clock recording is not limited to clear nights as are the light-detection methods. Consequently, radio antennas will be a valuable add-on for any air shower array targeting the energy range above 100 PeV.

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“…Limits on the fluxes of ultra-high-energy cosmic rays (left) and neutrinos (right) set by the NuMoon [14], RESUN [15] and LUNASKA Parkes [17] lunar Askaryan experiments, calculated as described in the text. Also shown are potential limits that could be set by future lunar Askaryan experiments with nominal observing times of 200 h with LOFAR [20,25], 200 h with a phased-array feed (PAF) on the Parkes radio telescope [26], or 2900 h with AuScope [18]. Shading shows the range of uncertainty associated with models of the small-scale lunar surface roughness; the discontinuity is an artefact of the model.…”

Section: Dedispersionmentioning

confidence: 99%

“…I estimate the limits or potential limits set by some past and near-future lunar Askaryan experiments using an analytic model for the particle aperture [18,23,24]. To reflect the effects of small-scale surface roughness, I use the only extant model [13], which represents the aperture as a linear combination of two extreme cases: one in which these effects are ignored, and one in which they are maximised, by representing the surface as a series of small-scale facets with uncorrelated slopes.…”

Section: Particle Sensitivitymentioning

confidence: 99%

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Sensitivity of lunar particle-detection experiments

Bray

2017

EPJ Web Conf.

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Abstract. The use of the Moon as a detector volume for ultra-high-energy neutrinos and cosmic rays, by searching for the Askaryan radio pulse produced when they interact in the lunar regolith, has been attempted by a range of projects over the past two decades. In this contribution, I discuss some of the technical considerations relevant to these experiments, and their consequent sensitivity to ultra-high-energy particles. I also discuss some possible future experiments, and highlight their potential.

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The wavelength variation of the granule/intergranule contrast

Cited by 9 publications

References 6 publications

Radio detection of cosmic-ray air showers and high-energy neutrinos

Radio detection of cosmic-ray air showers and high-energy neutrinos

Status of air-shower measurements with sparse radio arrays

Sensitivity of lunar particle-detection experiments

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