Cosmic rays from the knee to the highest energies

Blümer, J.; Engel, R.; Hörandel, J. R.

doi:10.1016/j.ppnp.2009.05.002

Cited by 277 publications

(212 citation statements)

References 470 publications

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“…Sometimes, gamma rays and neutrinos do not count as cosmic rays, because the cosmic accelerators are believed to accelerate only charged particles, and thus any uncharged particle ought to be a secondary product of a charged primary cosmic ray particle. Even today, it is not totally clear what the sources of cosmic rays are and which mechanism is responsible for the acceleration of cosmic rays at the highest energies [4].…”

Section: Cosmic Raysmentioning

confidence: 99%

“…Figure 2.1.: Cosmic ray energy spectrum from exemplary chosen direct balloon and satellite experiments, and indirect air shower based measurements [4].…”

Section: Origin Of Cosmic Raysmentioning

confidence: 99%

“…However, recent theoretical studies revealed that this is only a minor contribution [33], and it is still under investigation by which degree it influences the total radio emission by air showers. 4. Variation of the net charge excess (Askaryan effect [27]):…”

Section: Variation Of the Dipole Strength Of The Air Shower [40]mentioning

confidence: 99%

“…The positions of the LOPES antennas have been measured with differential GPS, in a coordinate system (see table 4.1) pointing towards geographic North, which deviates from the magnetic North by a about 1 • (see e.g., [84]). This magnetic declination has changed slightly over the run time of LOPES, and is ignored in the calibration and analysis, as it is small compared to other systematic errors.…”

Section: Measurement Of Antenna Positionsmentioning

confidence: 99%

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Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Schröder¹

2012

Springer Theses

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Instruments and Methods for the Radio Detection of High Energy Cosmic RaysCosmic rays at energies above 10 15 eV cannot be measured directly due to the low flux. Instead, the properties of the primary cosmic ray particles (arrival direction, energy, mass) have to be reconstructed from measurements of secondary particles forming an air shower. For this, digital radio antenna arrays, like LOPES at the Karlsruhe Institute of Technology (KIT), are a relatively new instrument. The radio emission mainly originates from the deflection of secondary air shower electrons and positrons in the Earth's magnetic field. The radio technique aims at achieving a similar quality in the reconstruction of air shower parameters as the established Cherenkov or fluorescence light detection methods, which in contrast to the radio technique are limited to dark, moonless nights.The present studies aim to advance the air shower radio detection in technological aspects and analysis methods. The developments are mainly applied to LOPES, but also provide a useful set of tools, which will soon be applied on the analysis of first AERA measurements. AERA is a next generation digital radio array at the Pierre Auger Observatory in Argentina. Moreover, this thesis reflects the recent progress in the understanding of the radio emission by air showers. The main results of the studies are:• A new method for time calibration with a reference beacon has been developed.It allows a time resolution of ∼ 1 ns even with large antenna arrays. This is necessary for digital radio interferometry which improves the signal-to-noise ratio and the reconstruction accuracy of the primary particle properties. This method is essential for the measurement of cosmic rays with LOPES, and is going to be applied at AERA.• A per-event comparison of lateral distributions measured with LOPES and REAS3 simulations reflects a significantly improved understanding of the radio emission mechanisms. For the first time a Monte Carlo simulation of the radio emission by air showers can in average reproduce measured data. A detailed investigation of systematic effects was performed to accurately reconstruct LOPES lateral distributions. In particular, a method has been developed to appropriately treat the influence of radio noise on measured lateral distributions.• It is shown that a conical radio wavefront fits LOPES measurements and REAS3 simulations better than a spherical wavefront, which up to now has been assumed for LOPES beamforming analyses. Furthermore, the atmospheric depth of the shower maximum X max can be reconstructed by determining the opening angle of the conical wavefront. However, due to the small lateral extension of LOPES of about 200 m and the high radio background at KIT, the measurement uncertainty (∆X max ≈ 200 g/cm 2 ) is too large for a per-event reconstruction of the primary mass. This will improve at AERA, but could not be examined in detail because of a delay in the construction. • Eine neue Methode zur Zeitkalibration mit einen Rerefenzsender (Beaco...

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Section: Cosmic Raysmentioning

confidence: 99%

“…Figure 2.1.: Cosmic ray energy spectrum from exemplary chosen direct balloon and satellite experiments, and indirect air shower based measurements [4].…”

Section: Origin Of Cosmic Raysmentioning

confidence: 99%

Section: Variation Of the Dipole Strength Of The Air Shower [40]mentioning

confidence: 99%

Section: Measurement Of Antenna Positionsmentioning

confidence: 99%

See 2 more Smart Citations

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Schröder¹

2012

Springer Theses

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“…Unfortunately, cosmic rays can be measured only indirectly above an energy of 10 14 eV, through the cascades of secondary particles, called extensive air showers (EAS), that they produce in the atmosphere (for a recent review, see [1]). Only by simulating the generation of EAS and comparing the predictions with measurements can one draw conclusions on the primary mass composition of the arriving particles [2].…”

Section: Introductionmentioning

confidence: 99%

Review of Model Predictions for Extensive Air Showers

Pierog

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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In detailed air shower simulations, the uncertainty in the prediction of shower observable for different primary particles and energies is currently dominated by differences between hadronic interaction models. With the results of the first run of the LHC, the difference between post-LHC model predictions has been reduced at the same level as experimental uncertainties of cosmic ray experiments. At the same time new types of air shower observables, like the muon production depth, have been measured, adding new constraints on hadronic models. Currently no model is able to reproduce consistently all mass composition measurements possible with the Pierre Auger Observatory for instance. We review the current model predictions for various particle production observables and their link with air shower observables and discuss the future possible improvements.

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The new 4‐m robotic telescope

et al. 2019

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We present a project to build a 4-m-diameter telescope (New Robotic Telescope [NRT]) with fully robotic operation. The telescope will be sited at the Observatory of Roque de los Muchachos in the island of La Palma (Spain). When it enters into operation in 5 years' time, it will be likely the largest robotic telescope in the world. This, in conjunction with the extremely fast response and the versatile and flexible instrumentation in the optical and near-infrared ranges, will make the NRT a world-leading facility in the area of time-domain astrophysics. Here we discuss some of the main scientific cases, the mechanical and optical design, the control system, first light instrumentation, and the timeline of the project.

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Cosmic rays from the knee to the highest energies

Cited by 277 publications

References 470 publications

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Review of Model Predictions for Extensive Air Showers

The new 4‐m robotic telescope

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