Investigation of long-time cosmic-ray variations

1968 ◽  
Vol 46 (10) ◽  
pp. S907-S910
Author(s):  
R. B. Salimzibarov ◽  
V. D. Sokolov ◽  
N. G. Skryabin ◽  
V. V. Klimenko ◽  
Yu. G. Shafer
Keyword(s):  
Experimental Data ◽  
Cosmic Rays ◽  
Ionization Chamber ◽  
Cosmic Ray ◽  
Charge Composition ◽  
Annual Variations ◽  
Long Time

During 1958–66 the flux and mean ionization chamber response of cosmic-ray particles were measured. On the basis of the experimental data the 11-year variations of the flux and of the charge composition of cosmic rays, and the annual variations, have been investigated.

scholarly journals High energy cosmic ray interactions and UHECR composition problem

2019 ◽  
Vol 210 ◽  
pp. 02001
Author(s):  
Sergey Ostapchenko
Keyword(s):  
Experimental Data ◽  
Monte Carlo ◽  
Cosmic Rays ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Hadronic Interactions ◽  
High Energy Cosmic Rays ◽  
Cosmic Ray Interactions ◽  
Composition Problem

The differences between contemporary Monte Carlo generators of high energy hadronic interactions are discussed and their impact on the interpretation of experimental data on ultra-high energy cosmic rays (UHECRs) is studied. Key directions for further model improvements are outlined. The prospect for a coherent interpretation of the data in terms of the UHECR composition is investigated.

scholarly journals The nature of large cosmic-ray bursts

1936 ◽  
Vol 154 (881) ◽  
pp. 223-245 ◽  
Keyword(s):  
Cosmic Rays ◽  
Ionization Chamber ◽  
Cosmic Ray ◽  
Conclusive Evidence ◽  
Recording Apparatus ◽  
Ionization Current ◽  
Continuous Record ◽  
Normal Fluctuations

A continuous record of the ionization current produced by cosmic rays in an ionization chamber shows, if the recording apparatus is sufficiently sensitive, occasional relatively large momentary currents superposed on the normal fluctuations. These large momentary currents are generally called “bursts”. They were first discovered by Hoffmann. It has often been assumed that the bursts are of the same nature as the showers which are observed either in the Wilson chamber or by means of three or more coincidence counters; but so far no conclusive evidence, particularly for the larger bursts, has been reported in support of this assumption.

scholarly journals Cosmic ray spectra in planetary atmospheres

2008 ◽  
Vol 4 (S257) ◽  
pp. 471-473
Author(s):  
M. Buchvarova ◽  
P. Velinov
Keyword(s):  
Experimental Data ◽  
Solar Cycle ◽  
Cosmic Rays ◽  
Cosmic Ray ◽  
Planetary Atmospheres ◽  
Galactic Cosmic Rays ◽  
Outer Planets ◽  
Practical Possibility ◽  
The Earth ◽  
Theoretical Results

AbstractOur model generalizes the differential D(E) and integral D(>E) spectra of cosmic rays (CR) during the 11-year solar cycle. The empirical model takes into account galactic (GCR) and anomalous cosmic rays (ACR) heliospheric modulation by four coefficients. The calculated integral spectra in the outer planets are on the basis of mean gradients: for GCR – 3%/AU and 7%/AU for anomalous protons. The obtained integral proton spectra are compared with experimental data, the CRÈME96 model for the Earth and theoretical results of 2D stochastic model. The proposed analytical model gives practical possibility for investigation of experimental data from measurements of galactic cosmic rays and their anomalous component.

scholarly journals Atmospheric effects of the cosmic-ray mu-meson component

2018 ◽  
Vol 4 (3) ◽  
pp. 76-82 ◽  
Author(s):  
Валерий Янчуковский ◽  
Valery Yanchukovsky ◽  
Василий Кузьменко ◽  
Vasiliy Kuzmenko
Keyword(s):  
Experimental Data ◽  
Factor Analysis ◽  
Cosmic Rays ◽  
Theoretical Calculations ◽  
Cosmic Ray ◽  
Atmospheric Effects ◽  
Atmospheric Component ◽  
Significant Temperature ◽  
Muon Intensity ◽  
Barometric Effect

Variations in the intensity of cosmic rays observed in the depth of the atmosphere include the atmospheric component of the variations. Cosmic-ray muon telescopes, along with the barometric effect, have a significant temperature effect due to the instability of detected particles. To take into account atmospheric effects in muon telescope data, meteorological coefficients of muon intensity are found. The meteorological coefficients of the intensity of muons recorded in the depth of the atmosphere are estimated from experimental data, using various methods of factor analysis. The results obtained from experimental data are compared with the results of theoretical calculations.

scholarly journals 39. The anisotropy of primary cosmic radiation and the electromagnetic state in interplanetary space

1958 ◽  
Vol 6 ◽  
pp. 377-385
Author(s):  
V. Sarabhai ◽  
N. W. Nerurkar ◽  
S. P. Duggal ◽  
T. S. G. Sastry
Keyword(s):  
Experimental Data ◽  
Cosmic Rays ◽  
Cosmic Radiation ◽  
Interplanetary Space ◽  
Daily Variation ◽  
Cosmic Ray ◽  
The Sun ◽  
Cosmic Ray Intensity ◽  
Daily Variations ◽  
Primary Cosmic Radiation

Study of the anisotropy of cosmic rays from the measurement of the daily variation of meson intensity has demonstrated that there are significant day-today changes in the anisotropy of the radiation. New experimental data pertaining to these changes and their solar and terrestrial relationships are discussed.An interpretation of these changes of anisotropy in terms of the modulation of cosmic rays by streams of matter emitted by the sun is given. In particular, an explanation for the existence of the recently discovered types of daily variations exhibiting day and night maxima respectively, can be found by an extension of some ideas of Alfvén, Nagashima, and Davies. An integrated attempt is made to interpret the known features of the variation of cosmic ray intensity in conformity with ideas developed above.

scholarly journals INFLUENCE OF THE RESULTS OF UHECR DETECTION ON THE LHC EXPERIMENTS

2013 ◽  
Vol 53 (A) ◽  
pp. 707-711 ◽  
Author(s):  
Anatoly A. Petrukhin
Keyword(s):  
Experimental Data ◽  
Cosmic Rays ◽  
Energy Region ◽  
Center Of Mass ◽  
Cosmic Ray ◽  
Theoretical Models ◽  
Energy Interval ◽  
Mass System ◽  
New Approaches ◽  
Region 10

The cosmic ray energy region 10<sup>15</sup> ÷ 10<sup>17</sup>TeV corresponds to LHC energies 1 ÷ 14TeV in the center-of-mass system. The results obtained in cosmic rays (CR) in this energy interval can therefore be used for developing new approaches to the analysis of experimental data, for interpreting the results, and for planning new experiments. The main problem in cosmic ray investigations is the remarkable excess of muons, which increases with energy and cannot be explained by means of contemporary theoretical models. Some possible new explanations of this effect and other unusual phenomena observed in CR, and ways of searching for them in the LHC experiments are discussed.

scholarly journals Supernova remnants and the origin of cosmic rays

2013 ◽  
Vol 9 (S296) ◽  
pp. 305-314
Author(s):  
Jacco Vink
Keyword(s):  
Synchrotron Radiation ◽  
Cosmic Rays ◽  
Magnetic Fields ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Long Time ◽  
Gamma Ray Emission

AbstractSupernova remnants have long been considered to be the dominant sources of Galactic cosmic rays. For a long time the prime evidence consisted of radio synchrotron radiation from supernova remnants, indicating the presence of electrons with energies of several GeV. However, in order to explain the cosmic ray energy density and spectrum in the Galaxy supernova remnant should use 10% of the explosion energy to accelerate particles, and about 99% of the accelerated particles should be protons and other atomic nuclei.Over the last decade a lot of progress has been made in providing evidence that supernova remnant can accelerate protons to very high energies. The evidence consists of, among others, X-ray synchrotron radiation from narrow regions close to supernova remnant shock fronts, indicating the presence of 10-100 TeV electrons, and providing evidence for amplified magnetic fields, gamma-ray emission from both young and mature supernova remnants. The high magnetic fields indicate that the condition for accelerating protons to >1015 eV are there, whereas the gamma-ray emission from some mature remnants indicate that protons have been accelerated.

IONIZATION LOSS BY COSMIC-RAY MU-MESONS IN ARGON

1959 ◽  
Vol 37 (2) ◽  
pp. 189-202 ◽  
Author(s):  
Georges Hall
Keyword(s):  
Experimental Data ◽  
Energy Loss ◽  
Ionization Chamber ◽  
Cosmic Ray ◽  
Statistical Distribution ◽  
Experimental Curve ◽  
Energy Losses ◽  
Ionization Loss ◽  
Electron Collection ◽  
Probable Loss

The ionization of argon by cosmic-ray mu-mesons of minimum specific ionization has been studied by means of a calibrated pressure-ionization chamber using electron collection. Corrections which are shown to be necessary have been applied to the experimental data. The shape of the experimental curve of statistical distribution of energy loss agrees with the theoretically predicted shape, for energy losses greater than the most probable loss (300 kev).

scholarly journals Meson formation and the geomagnetic effects

1947 ◽  
Vol 192 (1028) ◽  
pp. 99-114 ◽  
Keyword(s):  
Experimental Data ◽  
Quantitative Analysis ◽  
Cosmic Rays ◽  
Charged Particles ◽  
Meson Production ◽  
Cosmic Ray ◽  
Average Multiplicity ◽  
Soft Component ◽  
Positively Charged ◽  
Mode Of Production

The experimental data on the cosmic-ray geomagnetic effects are used to provide information on the nature of the primary cosmic rays and on the mode of production of the meson component. The relevant arguments are first reviewed in a qualitative way and then elaborated by a quantitative analysis, which is not dependent upon any specific theory of meson production. Three main possibilities are discussed, the so-called proton, ‘mixed’ and soft component hypotheses (see §1 for definitions). It is concluded that the bulk of the mesons must arise from protons (or possibly other heavier positively charged particles). The analysis suggests that the average multiplicity of the process of meson production is about nine. From consideration of the asymmetry at high altitudes it seems likely that the primary radiation consists of protons and electrons (equally positive and negative) in the ratio of about one proton to four electrons.

THE ALTITUDE EFFECT ON THE SPECIFIC IONIZING POWER AND ZENITH ANGLE DISTRIBUTION OF COSMIC RAYS

1938 ◽  
Vol 16a (2) ◽  
pp. 29-40 ◽  
Author(s):  
Darol K. Froman ◽  
J. C. Stearns
Keyword(s):  
Cosmic Rays ◽  
Zenith Angle ◽  
Ionization Chamber ◽  
Unit Area ◽  
Cosmic Ray ◽  
Angle Distribution ◽  
Altitude Effect ◽  
Counting System ◽  
Chamber Measurements ◽  
Zenith Angle Distribution

Measurements made with a quadruple-coincidence Geiger-Müller counting system at altitudes of 120 and 14,160 ft. give the intensity, J, of cosmic ray ionizing particles at various zenith angles, ψ. The distribution, J(ψ) = J0e−0.175ψ cos2ψ, does not differ significantly from any measured values, and agrees with all observations within 0.5 and 3.0% of the vertical intensities at the lower and higher altitudes respectively. The total number of rays incident per unit area per unit time was found, and the specific ionization was determined by comparison with ionization chamber measurements. The results are given below.[Formula: see text]† Ionization chamber data from Clay and Jongen (4).* Ionization chamber data from Millikan and Cameron (18).

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