scholarly journals Multi-wavelength observation of cosmic-ray air-showers with CODALEMA/EXTASIS

2019 ◽  
Vol 210 ◽  
pp. 05003
Author(s):  
Antony Escudie ◽  
Didier Charrier ◽  
Richard Dallier ◽  
Daniel García-Fernández ◽  
Alain Lecacheux ◽  
...  
Keyword(s):  
Electric Field ◽  
Strong Electric Field ◽  
Radio Pulse ◽  
Cosmic Ray ◽  
Ground Level ◽  
Air Showers ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Multi Wavelength ◽  
Electric Field Profile

Since 2003, significant efforts have been devoted to the understanding of the radio emission of extensive air shower in the range [20-200] MHz. Despite some studies led until the early nineties, the [1-10] MHz band has remained unused for 20 years. However, it has been measured by some pioneering experiments that extensive air shower emit a strong electric field in this band and that there is evidence of a large increase in the amplitude of the radio pulse at lower frequencies. The EXTASIS experiment, located within the Nançay Radioastronomy Observatory and supported by the CODALEMA experiment, aims to reinvestigate the [1-10] MHz band, and especially to study the so-called “Sudden Death” contribution, the expected electric field emitted by shower front when hitting the ground level. Currently, EXTASIS has confirmed some results obtained by the pioneering experiments, and tends to bring explanations to the other ones, for instance the role of the underlying atmospheric electric field. Moreover, CODALEMA has demonstrated that in the most commonly used frequency band ([20-80] MHz) the electric field profile of EAS can be well sampled, and contains all the information needed for the reconstruction of EAS: an automatic comparison between the SELFAS3 simulations and data has been developed, allowing us to reconstruct in an almost real time the primary cosmic ray characteristics.

RADIO DETECTION OF COSMIC RAYS WITH LOPES

2006 ◽  
Vol 21 (supp01) ◽  
pp. 168-181 ◽  
Author(s):  
A. HORNEFFER ◽  
W. D. APEL ◽  
F. BADEA ◽  
L. BÄHREN ◽  
K. BEKK ◽  
...  
Keyword(s):  
Radio Pulse ◽  
Pulse Height ◽  
Cosmic Ray ◽  
Radio Interference ◽  
Air Showers ◽  
Digital Radio ◽  
Radio Receivers ◽  
Air Shower ◽  
Radio Detection ◽  
Digital Radio Receivers

Measuring radio pulses from cosmic ray air showers offers various new opportunities. New digital radio receivers allow measurements of these radio pulses even in environments that have lots of radio interference. With high bandwidth ADCs and fast data processing it is possible to store the whole waveform information in digital form and analyse transient events like air showers even after they have been recorded. Digital filtering and beam forming can be used to suppress the radio interference so that it is possible to measure the radio pulses even in radio loud environments. LOPES is a prototype station for the new digital radio interferometer LOFAR and is tailored to measure air showers. For this it is located at the site of the KASCADE-Grande air shower experiment. Already with the first phase of LOPES we have been able to measure radio pulses from air showers and show correlations between the radio pulse height and air shower parameters. The first part gives an introduction and presents the science results of LOPES, while the second part presents the hard- and software that enables LOPES to detect air short pulses.

scholarly journals Extensive Air Showers and Radio Frequency Electromagnetic Fields

1978 ◽  
Vol 31 (5) ◽  
pp. 439 ◽  
Author(s):  
K Sivaprasad
Keyword(s):  
Electric Field ◽  
Electromagnetic Fields ◽  
Weather Conditions ◽  
Geoelectric Field ◽  
Production Mechanism ◽  
Frequency Range ◽  
Air Showers ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Shower Development

An estimate is made of the electric field expected from the ionization electrons produced by an extensive air shower moving in the geoelectric field for frequencies from 10 kHz to 10 MHz. The calculations are for a geoelectric production mechanism, and they invoke quite reasonable assumptions regarding the shower development. The calculated fields are found to be comparable with those produced by the geomagnetic mechanism, and fall short of the high values observed in this frequency range. Higher fields cannot be obtained from the present shower mechanism under normal weather conditions, but would require exceptionally large values for the geoelectric field (1 MVm-1) or a model for electron diffusion that is radically different from that assumed here.

scholarly journals Sub-TeV hadronic interaction model differences and their impact on air showers

2021 ◽  
Vol 81 (4) ◽  
Author(s):  
Á. Pastor-Gutiérrez ◽  
H. Schoorlemmer ◽  
R. D. Parsons ◽  
M. Schmelling
Keyword(s):  
Interaction Model ◽  
Cosmic Ray ◽  
Ground Level ◽  
Air Showers ◽  
Theoretical Frameworks ◽  
Hadronic Interaction ◽  
Interaction Models ◽  
Hadronic Interactions ◽  
Air Shower ◽  
Experimental Use

AbstractIn the sub-TeV regime, the most widely used hadronic interaction models disagree significantly in their predictions for post-first interaction and ground-level particle spectra from cosmic ray induced air showers. These differences generate an important source of systematic uncertainty in their experimental use. We investigate the nature and impact of model uncertainties through a simultaneous analysis of ground level particles and first interaction scenarios. We focus on air shower primaries with energies close to the transition between high and low energy hadronic interaction models, where the dissimilarities have been shown to be the largest and well within the range of accelerator measurements. Interaction models are shown to diverge as several shower scenarios are compared, reflecting intrinsic differences in the model theoretical frameworks. Finally, we discuss the importance of interactions in the energy regime where the switching between models occurs ($$<1$$ < 1  TeV) and the effect of the choice of model on the number of hadronic interactions within cosmic ray induced air showers of higher energies.

scholarly journals Extensive Air Shower Reconstruction using the timing information from the RF-system of the Astroneu array

2021 ◽  
Vol 2105 (1) ◽  
pp. 012018
Author(s):  
S Nonis ◽  
A Leisos ◽  
A Tsirigotis ◽  
G Bourlis ◽  
K Papageorgiou ◽  
...  
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Air Showers ◽  
Particle Detectors ◽  
Extensive Air Shower ◽  
High Energy Cosmic Rays ◽  
Air Shower ◽  
Timing Information ◽  
Rf Antennas ◽  
Rf Antenna

Abstract The Astroneu cosmic ray telescope is a distributed hybrid array consisting of both scintillator counters and RF antenna detectors used for the detection of extensive air showers (EAS). The array is deployed at the Hellenic Open University campus, on the outskirts of the urban area of Patras in Greece. In the present development phase, the Astroneu telescope includes two stations consisting of 3 scintillation detectors modules (SDM) and one RF antenna while a third station includes 3 particle detectors and 4 RF antennas (3SDM-4RF). In each station, the RF-detectors are operating receiving a common trigger upon a 3-fold coincidence between the particle detectors of the station. In this study we present recent results from the 3SDM-4RF autonomous station related to the estimation of the direction of the incoming cosmic air shower using only the timing information from the 4 RF detectors. The directions of the reconstructed showers using the RF timing are in agreement with the corresponding results using the SDMs timing as well as with the simulation predictions. This verifies that the RF signal emitted from EAS originating form Ultra High Energy Cosmic Rays (UHECR), can be detected even in areas with strong electromagnetic background.

The mechanism of the origin the NBE (CID) and the initiating event (IE) of lightning due to the volume phase wave of EAS-RREA synchronous ignition of streamer flashes

2020 ◽  
Author(s):  
Alexander Kostinskiy ◽  
Thomas Marshall ◽  
Maribeth Stolzenburg
Keyword(s):  
Electric Field ◽  
Runaway Electron ◽  
Strong Electric Field ◽  
Cosmic Ray ◽  
Relativistic Electrons ◽  
Runaway Electrons ◽  
Air Showers ◽  
Secondary Electrons ◽  
Lightning Initiation ◽  
Positive Streamer

&lt;p&gt;In an article by &lt;em&gt;Kostinskiy et al. (2019)&lt;/em&gt; proposed the mechanism of the origin and development of lightning from initiating event to initial breakdown pulses (termed the Mechanism). The Mechanism assumes initiation occurs in a region of a thundercloud of 1 km&lt;sup&gt;3&lt;/sup&gt; with electric field E &gt; 0.4 MV/(m&amp;#8729;atm), which contains, because of turbulence, numerous small &amp;#8220;E&lt;sub&gt;th&lt;/sub&gt;-volumes&amp;#8221; of 0.001-0.0001 m&lt;sup&gt;3&lt;/sup&gt; with E &amp;#8805; 3 MV/(m&amp;#8729;atm). The Mechanism allows for lightning initiation by two observed types of initiating events: a high power VHF event called an NBE (narrow bipolar event or CID), or a weak VHF event. According to the Mechanism, both types of initiating events are caused by a group of relativistic runaway electron avalanche particles passing through many of the E&lt;sub&gt;th&lt;/sub&gt;-volumes, thereby causing the nearly simultaneous launching of many positive streamer flashes, &lt;em&gt;Kostinskiy et al. (2019)&lt;/em&gt;.&lt;/p&gt;&lt;p&gt;In this report, based on the Meek&amp;#8217;s criterion for the initiation of streamers (&lt;em&gt;Raizer, 1991&lt;/em&gt;) at different heights of lightning initiation and taking into account the number of all background electrons, positrons and photons of cosmic rays with energy &amp;#949; &lt; 10&lt;sup&gt;12&lt;/sup&gt; eV (&lt;em&gt;Sato, 2015&lt;/em&gt;) crossing E&lt;sub&gt;th&lt;/sub&gt;-volumes sizes of E&lt;sub&gt;th&lt;/sub&gt;-volumes are specified (3&amp;#8729;10&lt;sup&gt;-4&lt;/sup&gt;-3&amp;#8729;10&lt;sup&gt;-5&lt;/sup&gt; m&lt;sup&gt;3&lt;/sup&gt;). The report also showed that synchronous injection with a high probability of relativistic electrons into such small E&lt;sub&gt;th&lt;/sub&gt;-volumes requires of relativistic runaway electrons avalanches to be initiated by extensive air showers with energies &amp;#949; &gt; 10&lt;sup&gt;15&lt;/sup&gt; eV, which would supply (injected) 10&lt;sup&gt;5&lt;/sup&gt;-10&lt;sup&gt;7&lt;/sup&gt; secondary electrons into a turbulent region of a thundercloud with a strong electric field.&lt;/p&gt;&lt;p&gt;References&lt;/p&gt;&lt;p&gt;Kostinskiy, A. Yu., Marshall, T.C., Stolzenburg, M. (2019), The Mechanism of the Origin and Development of Lightning from Initiating Event to Initial Breakdown Pulses arXiv:1906.01033&lt;/p&gt;&lt;p&gt;Raizer Yu. (1991), Gas Discharge Physics, Springer-Verlag, 449 p.&lt;/p&gt;&lt;p&gt;Sato T. (2015), Analytical Model for Estimating Terrestrial Cosmic Ray Fluxes Nearly Anytime and Anywhere in the World: Extension of PARMA/EXPACS, PLOS ONE, 10(12): e0144679.&lt;/p&gt;

SIMULATIONS OF EXTENSIVE AIR SHOWERS TRIGGERED BY PROTON, IRON AND GAMMA PRIMARIES

2005 ◽  
Vol 20 (29) ◽  
pp. 6814-6816
Author(s):  
A. GERANIOS ◽  
E. FOKITIS ◽  
S. MALTEZOS ◽  
K. PATRINOS ◽  
A. DIMOPOULOS
Keyword(s):  
Energy Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Extensive Air Showers ◽  
Ultra High Energy ◽  
Air Showers ◽  
Extensive Air Shower ◽  
Air Shower

Using the AIRES code, we have generated a large number of Extensive Air Showers corresponding to Ultra high energy cosmic ray gammas, protons and iron nuclei with energy range 1015 – 1022 eV. These simulations clearly show the different atmospheric depths of the Extensive Air Shower maxima in this energy range.

TeV ASTROPHYSICS WITH THE MILAGRO AND HAWC OBSERVATORIES

2013 ◽  
Vol 22 (11) ◽  
pp. 1360010
Author(s):  
◽  
GUS SINNIS
Keyword(s):  
Gamma Ray ◽  
Ground Level ◽  
Air Showers ◽  
Particle Detectors ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Transient Nature ◽  
High Duty Cycle ◽  
Order Of Magnitude ◽  
Enormous Number

Ground-based gamma-ray astronomy has historically implemented two dramatically different techniques. One method employs Imaging Atmospheric Cherenkov Telescope(s) (IACT) that detect the Cherenkov light generated in the atmosphere by extensive air showers. The other method employs particle detectors that directly detect the particles that reach ground level — known as Extensive Air Shower (EAS) arrays. Until recently, the IACT method had been the only technique to yield solid detections of TeV gamma-ray sources. Utilizing water Chernkov technology, Milagro, was the first EAS array to discover new gamma-ray sources and demonstrated the power of and need for an all-sky high duty cycle instrument in the TeV energy regime. The transient nature of many TeV sources, the enormous number of potential sources, and the existence of TeV sources that encompass large angular areas all point to the need for an all-sky, high duty-factor instrument with even greater sensitivity than Milagro. The High Altitude Water Cherenkov (HAWC) Observatory will be over an order of magnitude more sensitive than Milagro. In this paper we will discuss the results from Milagro and the design of the HAWC instrument and its experimental sensitivity.

scholarly journals Investigating the influence of diffractive interactions on ultrahigh-energy extensive air showers

2018 ◽  
Vol 33 (26) ◽  
pp. 1850153 ◽  
Author(s):  
L. B. Arbeletche ◽  
V. P. Gonçalves ◽  
M. A. Müller
Keyword(s):  
Phenomenological Models ◽  
Cosmic Ray ◽  
Extensive Air Showers ◽  
Ultrahigh Energy ◽  
Air Showers ◽  
Hadronic Interactions ◽  
Air Shower ◽  
Cosmic Ray Interactions ◽  
The Impact ◽  
Elasticity Number

The understanding of the basic properties of the ultrahigh-energy extensive air showers is dependent on the description of hadronic interactions in an energy range beyond that probed by the LHC. One of the uncertainties present in the modeling of air showers is the treatment of diffractive interactions, which are dominated by nonperturbative physics and usually described by phenomenological models. These interactions are expected to affect the development of the air showers, since they provide a way of transporting substantial amounts of energy deep in the atmosphere, modifying the global characteristics of the shower profile. In this paper, we investigate the impact of diffractive interactions in the observables that can be measured in hadronic collisions at high energies and ultrahigh-energy cosmic ray interactions. We consider three distinct phenomenological models for the treatment of diffractive physics and estimate the influence of these interactions on the elasticity, number of secondaries, longitudinal air shower profiles and muon densities for proton-air and iron-air collisions at different primary energies. Our results demonstrate that even for the most recent models, diffractive events have a non-negligible effect on the observables and that the distinct approaches for these interactions, present in the phenomenological models, still are an important source of theoretical uncertainty for the description of the extensive air showers.

scholarly journals Study of muons from ultrahigh energy cosmic ray air showers measured with the Telescope Array experiment

2019 ◽  
Vol 210 ◽  
pp. 02012
Author(s):  
R. Takeishi
Keyword(s):  
Interaction Model ◽  
Cosmic Ray ◽  
Mass Composition ◽  
Ultrahigh Energy ◽  
Air Showers ◽  
Hadronic Interaction ◽  
Telescope Array ◽  
Interaction Models ◽  
Air Shower ◽  
Number Of Particles

One of the uncertainties in ultrahigh energy cosmic ray (UHECR) observation derives from the hadronic interaction model used for air shower Monte-Carlo (MC) simulations. One may test the hadronic interaction models by comparing the measured number of muons observed at the ground from UHECR induced air showers with the MC prediction. The Telescope Array (TA) is the largest experiment in the northern hemisphere observing UHECR in Utah, USA. It aims to reveal the origin of UHECRs by studying the energy spectrum, mass composition and anisotropy of cosmic rays by utilizing an array of surface detectors (SDs) and fluorescence detectors. We studied muon densities in the UHE extensive air showers by analyzing the signal of TA SD stations for highly inclined showers. On condition that the muons contribute about 65% of the total signal, the number of particles from air showers is typically 1.88 ± 0.08 (stat.) ± 0.42 (syst.) times larger than the MC prediction with the QGSJET II-03 model for proton-induced showers. The same feature was also obtained for other hadronic interaction models, such as QGSJET II-04.

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