Measurement of the cosmic-ray iron spectrum between 60 and 200 GeV per nucleon

The nature of the asymmetrical showers at an energy of 200 GeV and the features of the pion interaction

Canadian Journal of Physics ◽

10.1139/p68-325 ◽

1968 ◽

Vol 46 (10) ◽

pp. S681-S683 ◽

Cited By ~ 1

Author(s):

I. N. Erofeeva ◽

L. G. Mishchenko ◽

V. S. Murzin ◽

L. I. Sarycheva

Keyword(s):

Pion Mass ◽

Center Of Mass ◽

Cosmic Ray ◽

Primary Energy ◽

Mass System ◽

Target Mass ◽

Considerable Portion ◽

Pion Interaction ◽

200 Gev ◽

Ionization Calorimeter

The nuclear interactions of nucleons and pions at an energy of 200 GeV have been studied using an ionization calorimeter, cloud chamber, and hodoscope units. It has been found that the showers which are asymmetrical backward have the two-peak angular distribution (on a log tan θ plot) and, in the center-of-mass system, the charged particles and neutrals appear in the remote and front hemispheres respectively. The showers which are asymmetrical forward are produced mainly by primary pions and are symmetrical in the system where the target mass is close to the pion mass. It is suggested that in the cosmic-ray energy range (e.g. at energies ~10 GeV), after interaction, a pion retains a considerable part of the primary energy, but may change its charge and be transmuted into a π0 meson. Such an assumption makes it possible to explain the considerable portion of the energy transferred to a photon in the pion interactions.

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Study of the solar anisotropy of cosmic ray primaries of about 200 GeV energy with the L3+C muon detector

Astronomy and Astrophysics ◽

10.1051/0004-6361:200809634 ◽

2008 ◽

Vol 488 (3) ◽

pp. 1093-1100

Author(s):

Keyword(s):

Cosmic Ray ◽

Muon Detector ◽

200 Gev

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The energy spectrum of primary cosmic ray electrons from 2 GeV to 200 GeV

Astrophysics and Space Science ◽

10.1007/bf00653319 ◽

1971 ◽

Vol 14 (2) ◽

pp. 301-313 ◽

Cited By ~ 11

Author(s):

J. L. Fanselow ◽

R. C. Hartman ◽

Peter Meyer ◽

P. J. Schmidt

Keyword(s):

Energy Spectrum ◽

Cosmic Ray ◽

200 Gev

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Quelques aspects de la physique des collisions noyau–noyau à énergie ultra relativiste

Canadian Journal of Physics ◽

10.1139/p89-203 ◽

1989 ◽

Vol 67 (12) ◽

pp. 1207-1218

Author(s):

Claude Leroy

Keyword(s):

Transverse Energy ◽

Lattice Gauge Theory ◽

Nuclear Research ◽

Cosmic Ray ◽

High Energy ◽

European Organization ◽

Lattice Gauge ◽

200 Gev ◽

Normal Nuclear Density ◽

Order Of Magnitude

We discuss the results of the measurements of the energy flow and multiplicity for the collisions of 16O and 32S with a set of target nuclei at an incident energy of 60 and 200 GeV/nucleon and 200 GeV/nucleon, respectively. These measurements have been performed at the European Organization for Nuclear Research (CERN) super proton synchroton by NA-34/HELIOS (high energy lepton and ion spectrometer), NA-35, NA-36, NA-38, and WA-80 in various pseudorapidity regions. The measurements of the transverse energy (ET) distributions provide an understanding of the concept of the stopping power and the estimates of the energy density reached. The energy densities reached in these collisions (~ 5 GeV/fm3) are at least an order of magnitude larger than the normal nuclear density (0.15 GeV/fm3) and are also in the region of the critical value of ~ 2.5 GeV/fm3 obtained from lattice gauge theory. [Formula: see text], obtained by combining the transverse energy and the multiplicity measurements, is compared with earlier results reported in cosmic-ray studies. The pT spectra of the charged particles and photons produced in these collisions are compared with the corresponding spectra measured in proton–nucleus collisions. The present situation suggests the study of new observables.

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Correlation Between the Cosmic-ray Solar Daily Variation Underground and Geomagnetic Activity

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000011140 ◽

1968 ◽

Vol 1 (4) ◽

pp. 149-150

Author(s):

A. G. Fenton

Keyword(s):

Cosmic Ray ◽

High Energy ◽

Particle Energy ◽

Primary Spectrum ◽

The Earth ◽

Low Energies ◽

200 Gev ◽

Surface Muon ◽

Meteorological Influences ◽

The University

Since 1957, the University of Tasmania has operated cosmic-ray meson telescopes at an underground site near Hobart for the purpose of monitoring the intensity variations in the high energy component of the primary flux near the Earth. Details relating to the site, equipment, and meteorological influences on the observed intensity have been given previously. At a depth equivalent to 36m of water (36 m.w.e.), the equipment responds to an effective primary spectrum having a mean particle energy in the vicinity of 200 GeV and falling off rapidly at low energies, so that about 90% of the primaries have energy exceeding 50 GeV. The corresponding mean energy of response for surface muon telescopes at Hobart is about 25 GeV, while a neutron monitor at Hobart has a mean response at about 7 GeV.

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Sidereal time variation of high-energy cosmic rays observed by an air Cerenkov telescope

Canadian Journal of Physics ◽

10.1139/p68-306 ◽

1968 ◽

Vol 46 (10) ◽

pp. S607-S610 ◽

Cited By ~ 5

Author(s):

Y. Sekido ◽

K. Nagashima ◽

I. Kondo ◽

T. Murayama ◽

H. Okuda ◽

...

Keyword(s):

Cosmic Rays ◽

Cosmic Ray ◽

High Energy ◽

Sidereal Time ◽

High Energy Cosmic Rays ◽

Four Seasons ◽

200 Gev ◽

The Difference ◽

Celestial Sphere ◽

Sidereal Anisotropy

Using the cosmic-ray telescope No. 3 (air Cerenkov telescope) at Nagoya, observations of high-energy (~200 GeV) cosmic rays were continued during the period from February 1964 to March 1966. The observations were made at a fixed zenith angle Z = 60° and at two azimuths A = 72° and 288°. With this setting, the celestial sphere was scanned in the declination band between 25° and 40 °N. Using the difference between the two diurnal vectors observed at 72° (east) and 288° (west), the anisotropy, free from any diurnal variation of meteorological origin, was obtained corresponding to each of four seasons. From these four anisotropy vectors, the solar anisotropy was found to be insignificant, but the sidereal anisotropy was as follows:[Formula: see text]

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The future of the high energy cosmic ray detection: HERD

EPJ Web of Conferences ◽

10.1051/epjconf/201920901040 ◽

2019 ◽

Vol 209 ◽

pp. 01040

Author(s):

Chiara Perrina

Keyword(s):

Cosmic Rays ◽

Gamma Ray ◽

Direct Detection ◽

Radiation Detection ◽

Space Station ◽

Cosmic Ray ◽

Life Time ◽

High Energy ◽

The Future ◽

200 Gev

The High Energy cosmic-Radiation Detection (HERD) facility will be one of the space astronomy payloads on board the future Chinese space station. The ambitious aim of HERD is the direct detection of cosmic rays towards the “knee” region (~ 1 PeV), with a detector able to measure electrons, photons and nuclei with an excellent energy resolution (1% for electrons and photons at 200 GeV and 20% for nuclei at 100 GeV - PeV), an acceptance 10 times the one of present generation missions (~ 1 m2 sr), and long life-time (> 10 years). The primary objectives of HERD are the indirect search for dark matter particles and the precise measurement of energy distribution and composition of cosmic rays from 30 GeV up to a few PeV, determining the origin of the “knee” structure of the spectrum. Furthermore, HERD will monitor the high energy gamma-ray sky from 500 MeV, observing gamma-ray bursts, active galactic nuclei, galactic microquasars, etc. HERD will be composed of a homogeneous calorimeter, surrounded by a particle tracker and a plastic scintillator detector. Two possible trackers are under study: a 5-side tracker made of silicon strip detectors and a 4-side scintillating fiber tracker with a silicon strip top tracker. The total volume of HERD will be (2.3 × 2.3 × 2.6) m3 with a weight of about 4 t. The HERD design, perspectives, expected performances in terms of energy sensitivity and acceptance will be presented in this contribution.

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