Simple coincidence technique for cosmic-ray intensity exploration via low-energy photon detection

The results of the analysis of data obtained from measurements carried out by means of regular stratospheric launchings of cosmic-ray radiosondes over the Murmansk region and the Antarctic observatory in Mirny in 1963–66 are presented. The problem of the anisotropy of the primary component of low-energy cosmic rays and of temperature effects on the cosmic-ray intensity in the atmosphere are discussed.

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Low-Energy Photon Detection with PWO-II Scintillators and Avalanche Photodiodes in Application to High-Energy Gamma-Ray Calorimetry

Advances in Photodiodes ◽

10.5772/14191 ◽

2011 ◽

Author(s):

Dmytro Melnychuk ◽

Boguslaw Zwieglinski

Keyword(s):

Gamma Ray ◽

Avalanche Photodiodes ◽

High Energy ◽

Low Energy ◽

Energy Photon ◽

Photon Detection ◽

High Energy Gamma ◽

Energy Gamma

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HIGH-ALTITUDE COSMIC RAY MEASUREMENTS AT FORT CHURCHILL

Canadian Journal of Physics ◽

10.1139/p60-069 ◽

1960 ◽

Vol 38 (5) ◽

pp. 638-641 ◽

Cited By ~ 1

Author(s):

I. B. McDiarmid ◽

D. C. Rose

Keyword(s):

Solar Activity ◽

High Altitude ◽

Solar Minimum ◽

Solar Maximum ◽

Cosmic Ray ◽

Geiger Counter ◽

Low Energy ◽

High Solar Activity ◽

Energy Radiation ◽

Cosmic Ray Intensity

Measurements with rocket-borne Geiger counters have been carried out at altitudes up to 250 km at Fort Churchill, Manitoba. The total primary cosmic ray intensity at a time near a solar maximum has been determined and compared with other measurements taken at times of high solar activity and also with other Geiger counter measurements obtained near a solar minimum. A low-energy radiation was observed whose intensity increased with altitude up to about 25% of the primary intensity at 250 km.

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Two anisotropies of the cosmic-ray particles producing the cosmic-ray diurnal variation

Canadian Journal of Physics ◽

10.1139/p68-361 ◽

1968 ◽

Vol 46 (10) ◽

pp. S828-S830

Author(s):

Masatoshi Kitamura

Keyword(s):

Cosmic Rays ◽

Diurnal Variation ◽

Interplanetary Space ◽

Geomagnetic Latitude ◽

Cosmic Ray ◽

Diurnal Variations ◽

Low Energy ◽

The Other ◽

Energy Spectra ◽

Cosmic Ray Intensity

The solar diurnal variations of both meson and nucleon components of cosmic rays at sea level at geomagnetic latitude 57.5° and geomagnetic longitude 0° are analyzed by the model in which two anisotropies of cosmic-ray particles (one of them, Δj1, from about 20 h L.T. and the other, Δj2, from about 8 h L.T. in interplanetary space) produce the solar diurnal variation of the cosmic-ray intensity on the earth.When the energy spectra of Δj1 and Δj2 are represented by [Formula: see text] and [Formula: see text], respectively, where j0(E) is the normal energy spectrum of the primary cosmic rays, it is shown that the evaluation for m1 = 1, 2, m2 = 0 and the cutoffs at 8 and 10 BeV on the low-energy side of spectra of both Δj1 and Δj2 agree well with the observational results at Deep River.

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INTERPLANETARY AND SOLAR PLASMA PARAMETERS OF THE 14 JULY 2000 GROUND LEVEL ENHANCEMENT

International Journal of Modern Physics D ◽

10.1142/s0218271803002275 ◽

2003 ◽

Vol 12 (02) ◽

pp. 337-344 ◽

Cited By ~ 1

Author(s):

S. S. AL-THOYAIB

Keyword(s):

Rapid Change ◽

Cosmic Ray ◽

Ground Level ◽

Low Energy ◽

Neutron Monitors ◽

Ground Level Enhancement ◽

Plasma Parameters ◽

Cosmic Ray Intensity ◽

The Difference ◽

Galactic Cosmic Ray

The ground level enhancement (GLE) of 14 July 2000 observed in the cosmic ray intensity has been examined. The event was recorded only by neutron monitors. It has a complex intensity-time structure. The northern hemisphere stations (Thule, Goose Bay, and Oulu) recorded abrupt increases earlier by 10 minutes than those in the southern hemisphere. Due to the difference in sensitivity at rigidity less than ~3 GV, the considered detectors recorded different increases in count rates relative to galactic cosmic ray background. This paper presents the study of GLE associated with the X5.7 solar flare. The rapid change of arriving particles were anisotropic during the onset of the event; it become isotropic during the declining phase of the event, where only low energy protons remained. In addition, the observations of energetic solar particles and interplanetary parameters have been examined.

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