scholarly journals Extensive penetrating cosmic ray showers

1947 ◽  
Vol 191 (1027) ◽  
pp. 517-523 ◽  
Keyword(s):  
Cosmic Ray ◽  
Effective Density ◽  
Integral Spectrum ◽  
Number Of Particles

Extensive penetrating cosmic-ray showers were recorded with an arrangement consisting of a penetrating shower set P and an extension E containing shielded and unshielded counters. The following results were obtained: (1) The effective density integral spectrum of the showers observed is given by D ( x ) = Ax -0.5 , where x is the number of particles per m. 2 . (2) The rate of shower coincidences decreases only slightly when the extension is moved from a distance of 0.5 m. to a distance of 9 m. from the main set P . (3) The ratio of the coincidences obtained with shielded and unshielded extension counters does not change noticeably with increasing separation between E and P . The results are based on approximately 10,000 hr. of recording.

THE LOW ENERGY SPECTRUM OF COSMIC-RAY MESONS AT SEA LEVEL AT HIGH GEOMAGNETIC LATITUDES

1952 ◽  
Vol 30 (5) ◽  
pp. 373-387
Author(s):  
D. C. Rose ◽  
A. G. Voisin
Keyword(s):  
Canadian Arctic ◽  
Intensity Variation ◽  
Cosmic Ray ◽  
Small Variation ◽  
Low Energy ◽  
Coincidence Method ◽  
Integral Spectrum ◽  
The Third ◽  
Significant Difference ◽  
Number Of Particles

The differential range spectrum of cosmic-ray mesons has been measured by three different methods the first of which was used at two northern geomagnetic latitudes 56.8 (Ottawa) and 83.0 (Resolute in the Canadian Arctic). In the first method the integral spectrum was measured by absorption, and after various corrections the differential spectrum was derived. In the second method the number of particles stopped in a block of lead was measured by a coincidence–anticoincidence arrangement of counters. In the third method the delayed coincidence method was used, the meson being identified by its decay electron. Over the range studied (ranges in lead up to 700 gm∙per cm∙2) the results of the three methods are in general agreement and agree with others in that the smoothed data show only a small variation in intensity over the range studied. Some of the results suggest that a more detailed study of the spectrum might show some irregularities in the intensity variation with range. As would be expected no significant difference was found in the shape of the curves at the two stations.

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.

scholarly journals Linking supernovae and supernova remnants. Time-dependent injection in SN1987A and gamma-ray spectrum of IC443

2017 ◽  
Vol 12 (S331) ◽  
pp. 268-273
Author(s):  
O. Petruk ◽  
S. Orlando ◽  
M. Miceli
Keyword(s):  
Gamma Rays ◽  
Supernova Remnants ◽  
Gamma Ray ◽  
Supernova Explosion ◽  
Cosmic Ray ◽  
Proton Spectrum ◽  
Stationary Equation ◽  
Particle Injection ◽  
Particle Momentum ◽  
Number Of Particles

AbstractAcceleration times of particles responsible for the gamma-rays in supernova remnants (SNRs) are comparable with SNR age. If the number of particles starting acceleration was varying during early times after the supernova explosion then this variation should be reflected in the shape of the gamma-ray spectrum. In order to analyse this effect, we consider the time variation of the radio spectral index in SN1987A and solution of the non-stationary equation for particle acceleration. We reconstruct evolution of the particle injection in SN1987A, apply it to derive the particle momentum distribution in IC443 and model its gamma-ray spectrum. We show that: i) observed break in the proton spectrum around 50 GeV in IC443 is a consequence of the variation of the cosmic ray injection; ii) shape of the hadronic gamma-ray spectrum in SNRs critically depends on the temporal variation of the cosmic ray injection in the immediate post explosion phases.

scholarly journals Methods to measure the cosmic-ray composition with the Auger Engineering Radio Array

2019 ◽  
Vol 216 ◽  
pp. 02004 ◽  
Author(s):  
Fabrizia Canfora
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Mass Composition ◽  
Atmospheric Depth ◽  
Ultra High Energy ◽  
Air Showers ◽  
Radio Stations ◽  
High Energy Cosmic Rays ◽  
Air Shower ◽  
Number Of Particles

The mass composition of ultra-high-energy cosmic rays plays a key role in the understanding of the origins ofthese rare particles. A composition-sensitive observable is the atmospheric depth at which the air shower reaches the maximum number of particles (Xmax). The Auger Engineering Radio Array (AERA) detects the radio emission inthe 30-80 MHz frequency band from extensive air showers with energies larger than 1017 eV. It consists of more than 150 autonomous radio stations covering an area of about 17 km2. From the distribution of signals measured by the antennas, it is possible to estimate Xmax. In this contribution three independent methods for the estimation of Xmax will be presented.

scholarly journals COLOR GLASS CONDENSATE IN BRANE MODELS OR DON'T ULTRA HIGH ENERGY COSMIC RAYS PROBE 1015eV SCALE?

2005 ◽  
Vol 20 (06) ◽  
pp. 419-440 ◽  
Author(s):  
HOURI ZIAEEPOUR
Keyword(s):  
Cosmic Rays ◽  
Extra Dimension ◽  
Cosmic Ray ◽  
High Energy ◽  
Effective Density ◽  
Color Glass ◽  
Color Glass Condensate ◽  
Ultra High Energy ◽  
High Energy Cosmic Rays ◽  
Brane Models

In a previous work1 we have studied the propagation of relativistic particles in the bulk for some of the most popular brane models. Constraints have been put on the parameter space of these models by calculating the time delay due to propagation in the bulk of particles created during the interaction of Ultra High Energy Cosmic Rays (UHECRs) with protons in the terrestrial atmosphere. The question was, however, raised that probability of hard processes in which bulk modes can be produced is small and consequently, the tiny flux of UHECRs cannot constrain brane models. Here we use Color Glass Condensate (CGC) model to show that effects of extra dimensions are visible not only in hard processes when the incoming photon/parton hits a massive Kaluza–Klein mode but also through the modification of soft/semi-hard parton distribution. At classical level, for an observer in the CM frame of UHECR and atmospheric hadrons, color charge sources are contracted to a thin sheet with a width inversely proportional to the energy of the ultra energetic cosmic ray hadron and consequently they can see an extra dimension with comparable size. Due to QCD interaction, a short life swarm of partons is produced in front of the sheet and its partons can penetrate to the extra-dimension bulk. This reduces the effective density of partons on the brane or in a classical view creates a delay in the arrival of the most energetic particles if they are reflected back due to the warping of the bulk. In CGC approximation the density of swarm at different distances from the classical sheet can be related and therefore it is possible (at least formally) to determine the relative fraction of partons in the bulk and on the brane at different scales. Results of this work are also relevant to the test of brane models in hadron colliders like LHC.

scholarly journals Supernova Remnants and the ISM: Constraints from Cosmic-Ray Acceleration

1988 ◽  
Vol 101 ◽  
pp. 325-329
Author(s):  
Amri Wandel
Keyword(s):  
Supernova Remnants ◽  
Weak Shock ◽  
Cosmic Ray ◽  
Box Model ◽  
Effective Density ◽  
Moderate Amount ◽  
Supersonic Expansion ◽  
Cosmic Ray Acceleration ◽  
The Galaxy ◽  
Consistent Solution

AbstractSupernova remnants can reaccelerate cosmic rays and modify their distribution during the cosmic ray propagation in the galaxy. Cosmic ray observations (in particular the boron-to-carbon data) strongly limit the permitted amount of reacceleration, which is used to set an upper limit on the expansion of supernova remnants, and a lower limit on the effective density of the ISM swept up by supernova shocks. The constraint depends on the theory of cosmic ray propagation: the standard Leaky Box model requires a high effective density, > 1cm−3, and is probably inconsistent with the present picture of the ISM. Modifying the Leaky Box model to include a moderate amount of weak-shock reacceleration, a self consistent solution is found, where the effective density in this solution is ≈ 0.1 cm−3, which implies efficient evaporation of the warm ISM component by young supernova remnants, during most of their supersonic expansion.

IONIZING POWER OF COSMIC RAY PARTICLES AT SEA LEVEL

1951 ◽  
Vol 29 (6) ◽  
pp. 495-504 ◽  
Author(s):  
S. D. Chatterjee
Keyword(s):  
Sea Level ◽  
Distribution Curve ◽  
Pulse Height ◽  
Cosmic Ray ◽  
Relativistic Electrons ◽  
Height Distribution ◽  
Soft Component ◽  
Pulse Height Distribution ◽  
Counter Telescope ◽  
Number Of Particles

Using a proportional counter telescope arrangement, experiments have been carried out at sea level to explore the nature and ionizing power of particles in the soft component of cosmic radiation and those produced under 1.8 cm. and 20 cm. of lead. The results indicate a preponderance of relativistic electrons in the soft component and under 20 cm. of lead. Under 1.8 cm. of lead there is some disagreement with the calculated pulse height distribution curve but this can be attributed to the production of showers in the lead. These showers would obscure the presence of a small number of particles of unusually high ionizing power, if such exist.

scholarly journals The energy loss of penetrating cosmic-ray particles in copper

1938 ◽  
Vol 166 (927) ◽  
pp. 482-501 ◽  
Keyword(s):  
Energy Loss ◽  
Cosmic Ray ◽  
Low Energy ◽  
Complete Agreement ◽  
Absorption Properties ◽  
Extended Range ◽  
The Mean ◽  
Absorption Measurements ◽  
Made In ◽  
Number Of Particles

Absorption measurements for cosmic-ray particles by the cloud chamber method have been made in heavy metals by Anderson and Neddermeyer (1936), Crussard and Leprince Ringuet (1937), Blackett and Wilson (1937) and by Neddermeyer and Anderson (1937). Anderson and Neddermeyer have confined their attention to particles of low energy and give (1937) reasons for supposing that particles of differing absorption properties exist in this region ( E < 4 × 10 8 e-volts). This result is only partially confirmed by more recent work (Blackett 1938) which shows that for E < 2 × 10 8 e-volts the mean energy loss of all particles and the distribution of losses among the particles are in accord with the predicted behaviour of electrons, and that there is no appreciable number of particles at this energy with non-electronic absorption properties. It is only for energies above 2 × 10 8 e-volts that two different kinds of particle are found. In this region the very few absorbable particles are probably normal electrons, while the penetrating particles differ in some way from normal electrons but apparently become indistinguishable from them when the energy falls below about 2 × 10 8 e-volts. Measurements of the absorption of the particles in the region where penetrating particles predominate have been made by Blackett and Wilson over an extended range, while Crussard and Leprince Ringuet have measured the energy loss of particles of a mean energy about 8 × 10 8 e-volts and report a mean loss which is in accord with the measurements of Blackett and Wilson. Upon the nature of these penetrating particles there is not at present complete agreement. It is now generally believed that the particles are more massive than electrons and that they radiate according to the classical (Bethe-Heitler) formula appropriate to their mass.

scholarly journals Radio universality and template-based pulse synthesis

2019 ◽  
Vol 216 ◽  
pp. 03006
Author(s):  
David Butler ◽  
Tim Huege ◽  
Olaf Scholten
Keyword(s):  
Radio Emission ◽  
Analytical Modeling ◽  
Cosmic Ray ◽  
Simulation Studies ◽  
Air Showers ◽  
Particle Detection ◽  
One Dimensional ◽  
Air Shower ◽  
The One ◽  
Number Of Particles

When discussing radio emission from cosmic ray air showers we commonly make a number of assumptions regardingthe production and propagation physics. Incorporating all of these it should be possible to construct a forward model to predict the radio signal produced by an air shower from simple parameters, an application and generalisation of shower universality to radio emission. In terms of particle detection shower universality focuses on the one-dimensional longitudinal profile, counting only the number of particles. This appears insufficient in the context of radio emission, the particle cascade develops on the scale of traversed atmospheric depth while electromagnetic radiation scales with the geometric trajectories of the sources. Further a real shower extends several radio wavelengths in the lateral directionwhile analyses often assume a point source on the shower axis. Our simulation studies show an unanticipated complexity in the radio output responsible for around 10% variation in the signals. We are still in the process of identifying the relevant quantities and improving our analytical modeling accordingly.

scholarly journals The connexion between cosmic ray showers and bursts

1936 ◽  
Vol 155 (886) ◽  
pp. 532-545 ◽  
Keyword(s):  
Ionization Chamber ◽  
Ion Pairs ◽  
Cosmic Ray ◽  
Complete Information ◽  
Steel Frame ◽  
Linear Amplifier ◽  
The Mean ◽  
Commercial Nitrogen ◽  
Number Of Particles ◽  
Wire Cage

Cosmic ray showers have so far been mostly investigated by counting the number of triple coincidences of suitably arranged Geiger-Müller counters. The information obtained in this way is restricted to the number of these events and does not give the number of particles in the shower. To obtain more complete information on showers an ionization chamber was put above the counters in the experiments described below, and the ionization in the chamber was recorded whenever all three counters discharged simultaneously. 2- Experimental Arrangement The arrangement of ionization chamber and counters is seen from fig. 1. The ionization chamber proper consisted of a wire cage, rectangular in shape, of 2·1 liters volume, reinforced by a substantial steel frame. The inner electrode, connected to the first valve of a linear amplifier of the Wynn Williams type, was a plain wire net, also reinforced by a steel frame. The whole structure was put in a cylindrical brass vessel with a wall 3 mm thick, filled with commercial nitrogen at 5 atm. pressure. A potential of about- 1500 volts was maintained between the electrodes of the chamber, giving a field of 500 volts/cm. The collecting time of ions was calculated to be slightly under 1/50 sec. The mean path of a cosmic ray particle in the chamber is about 10 cm, in which distance on the average about 5000 I (ion pairs) are produced. The rate of single cosmic ray particles crossing the chamber is about 5 per second. These values are obtained under the assumption that in air at N. T. P., 2·48 I are produced by cosmic radiation per cm 3 and that a single particle produces produces 100 I per cm path in air at N. T. P. Fig. 1 shows also the size and arrangement of the counters and of the lead plate which is placed above the chamber to increase the number of showers.

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