The composition of low-energy cosmic rays in 1965

1968 ◽  
Vol 46 (10) ◽  
pp. S539-S543 ◽  
Author(s):  
D. E. Hagge ◽  
V. K. Balasubrahmanyan ◽  
F. B. McDonald
Keyword(s):  
Cosmic Rays ◽  
Energy Range ◽  
Cosmic Ray ◽  
Low Energy ◽  
Oxygen Flux ◽  
Energy Spectra ◽  
Solar Modulation ◽  
Charge Composition ◽  
Specific Component ◽  
Relative Abundances

Primary cosmic-ray energy spectra and charge composition have been measured during the 1965 period of solar modulation minimum. A dE/dx vs. E type of scintillator–photomultiplier detector on board the eccentric-orbiting NASA spacecraft OGO-I was used. The charge composition was measured through neon over an energy range of 25 to 200 MeV/nucleon, depending upon the specific component. The spectra for all groups are nearly flat during this time, with the oxygen flux at about 0.005 nucleus/(M2-sr-s-MeV/nucleon). The relative abundances found are Li, 0.27; Be, 0.11; B, 0.37; C, 1.20; N, 0.30; O 1.00; F, [Formula: see text]; Ne, 0 12 An L/M ratio of 0.30 ± 0.06 is found.

Low-energy cosmic-ray heavy nuclei during the time of solar minimum

1968 ◽  
Vol 46 (10) ◽  
pp. S598-S600
Author(s):  
E. Tamai ◽  
M. Tsubomatsu ◽  
K. Ogura
Keyword(s):  
Energy Range ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
Low Energy ◽  
Energy Spectra ◽  
Solar Modulation ◽  
Atmospheric Depth ◽  
Heavy Nuclei ◽  
Multiply Charged ◽  
Α Particles

Nuclear emulsions were exposed at 2.3 g cm−2 atmospheric depth over Fort Churchill in 1965. These emulsions have been examined for the tracks of multiply-charged [Formula: see text] nuclei, with emphasis being paid particularly to those particles that stopped in the emulsions. Differential energy spectra of α particles and [Formula: see text], [Formula: see text]and [Formula: see text] nuclei were obtained in the energy interval 60–550 MeV/nucleon. They represent experimental results during the period when solar modulation effects were at a minimum. The fluxes of α particles and L, M, and H nuclei for energy intervals of 60–170, 100–400, 100–525, and 140–550 MeV/nucleon were found to be 20.9 ± 1.2, 2.4 ± 0.4, 4.8 ± 0.6, and 2.5 ± 0.4 particles m−2 sr−1 s−1, respectively. The results also show that the L/M and H/M ratios at the top of the atmosphere were 0.56 ± 0.16 and 0.34 ± 0.13 respectively, in the energy range from 140 to 350 MeV/nucleon. These values are appreciably greater than those observed at higher energies.

scholarly journals CR-39 Plastic Track Detector Experiment for Measurement of Charge Composition of Primary Cosmic Rays

1981 ◽  
Vol 94 ◽  
pp. 37-38
Author(s):  
Y. V. Rao ◽  
A. Davis ◽  
M. P. Hagan ◽  
R. C. Filz
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Track Detector ◽  
Energy Spectra ◽  
Charge Composition ◽  
Significant Information ◽  
Residual Atmosphere ◽  
New Type ◽  
Air Force Base ◽  
Primary Cosmic Rays

A study of the relative abundances and energy spectra of heavy cosmic rays and isotopic composition in the region of Fe peak can yield significant information concerning their origin, acceleration and interstellar propagation. In recent years solid state nuclear track detectors have been employed extensively to study heavy primary cosmic rays. Plastic track detectors necessarily have large geometric factors for heavy primaries, and a continuous sensitivity for the duration of an extended exposure. A balloon-borne experiment consisting of 1 m2 passive detector array has been designed in order to obtain charge and energy spectra of primary cosmic rays in the region of Fe peak. Included in the array is a new type of nuclear-track-recording plastic, a polymer made from the monomer allyl diglycol carbonate (commercially known as CR-39). The stack was built as a set of nine modules. Three types of stack assembly was adopted for these modules: one consisting of ‘pure’ CR-39 plastic track detector: the next one, a composite assembly of CR-39 with three layers of 600 micron thick nuclear emulsions: and the last one with CR-39 and Lexan Polycarbonate. The payload was flown successfully in June 1979 from Eielson Air Force Base, Alaska. The flight was aloft for 3 hours 30 min at an average ceiling of 3 gm/cm2 of residual atmosphere. An attempt to stabilize and orient the payload utilizing a biaxial magnetometer combined with and electrical rotator was unsuccessful. The failure to orient the payload in a stable position would prevent us from determining the true direction of each cosmic ray particle and trace it backwards through the earth's magnetic field using a computer tracing program. Recovery of the payload was routine and all materials were in perfect condition.

scholarly journals Low Energy Cosmic Rays Emitted by the Orion Complex into the Local Medium

1997 ◽  
Vol 166 ◽  
pp. 187-190
Author(s):  
V. Schönfelder ◽  
V.A. Dogiel ◽  
M.J. Freyberg ◽  
G.E. Morfill
Keyword(s):  
Energy Balance ◽  
Cosmic Rays ◽  
Energy Range ◽  
Cosmic Ray ◽  
Low Energy ◽  
Powerful Source ◽  
Energy Deposit ◽  
Bremsstrahlung Emission ◽  
Local Medium ◽  
Galactic Cosmic Ray

AbstractThe excess of γ-ray emission in the energy range 3–7 MeV discovered by COMPTEL in the direction of the Orion complex may imply that there is a powerful source of low energy cosmic rays in the local galactic medium. Several interpretations of the excess have been suggested. One of them assumes that the emission is identified with nuclear de-excitation lines of excited 16O and 14C. To provide the excess the energy deposit in these nuclei should be as large as ~ 1039 erg s−1. If a comparable part of these nuclei escape into the local galactic medium they can play a significant role in the energy balance there.If the excess is interpreted as continuous it can be produced by bremsstrahlung emission of fast 10 MeV electrons. Much less energy deposit in these electrons is necessary (~ 1036 erg s−1) to generate the observed Orion flux. The intensity of these electrons even near Earth can be higher than that of the galactic cosmic ray electrons.

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

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.

Charge and energy spectra of cosmic-ray nuclei with Z = 10–28

1968 ◽  
Vol 46 (10) ◽  
pp. S588-S592 ◽  
Author(s):  
V. S. Bhatia ◽  
V. S. Chohan ◽  
S. D. Pabbi ◽  
S. Biswas
Keyword(s):  
Cosmic Rays ◽  
Nuclear Charge ◽  
Cosmic Ray ◽  
Energy Spectra ◽  
Charge Composition ◽  
Improved Method ◽  
Residual Atmosphere ◽  
Primary Ionization ◽  
Charge Determination

An improved method of charge determination of heavy primary cosmic rays of nuclear charge Z = 10–28 has been obtained by measuring the Fowler–Perkins parameter in less-sensitive G-2 and G-0 emulsions for the determination of the primary ionization. It is found that reliable measurements of the primary ionization can be made for ionizations as high as ~1 000 times minimum. The average errors in the charge determinations by this method were found to be about 0.5, 0.7, and 1.0 unit of charge for H1 (Z = 10–15), H2 (Z = 16–19), and H3 (Z = 20–30) groups of nuclei, respectively. This method has been applied to the study of the H1, H2, and H3 groups of nuclei in an emulsion stack exposed over Fort Churchill, Canada, on June 18, 1963 at 4.3 g cm−2 of residual atmosphere for 11.1 h. The results are based on an analysis of 340 nuclei with [Formula: see text]. The charge composition and relative abundances of the H1, H2, and H3 nuclei were obtained. The differential energy spectra of the H1, H2, H3, and [Formula: see text] groups of nuclei were determined in the energy interval 250–1 000 MeV/nucleon and integral fluxes for energy > 1 000 MeV/nucleon.

Differential energy spectra and intensity variation of 1-20 MeV/nucleon protons and helium nuclei in interplanetary space (1964-66)

1968 ◽  
Vol 46 (10) ◽  
pp. S498-S502 ◽  
Author(s):  
C. Y. Fan ◽  
G. Gloeckler ◽  
B. McKibben ◽  
K. R. Pyle ◽  
J. A. Simpson
Keyword(s):  
Solar Activity ◽  
Energy Range ◽  
Interplanetary Space ◽  
Intensity Variation ◽  
Low Energy ◽  
Energy Spectra ◽  
Solar Modulation ◽  
Space Probe ◽  
Solar Origin ◽  
Made In

Measurements made in interplanetary space with a ΔE-range telescope on the OGO I and OGO III satellites and on the Pioneer 7 space probe showed that protons and helium nuclei in the energy range I–20 MeV/nucleon are present during "quiet times" in late 1964, in May–October–November 1965, and in August 1966. The intensities for both proton and helium nuclei are found to decrease with increasing energies. The spectra join those of the particles above 20 MeV/nucleon, which are known to be of galactic origin. For both protons and helium nuclei, the fluxes were higher in the period of minimum solar modulation in 1965 than in 1964. While in 1966 the helium flux decreased to its 1964 level, the proton flux showed a further increase over this period. It is believed that most of the particles observed during the period of minimum solar modulation were of galactic origin. As solar activity increases again, it seems that to the galactic low-energy fluxes, particularly for protons, there is added a steady contribution of solar origin.

The results of simultaneous measurements of the cosmic-ray intensity over the Antarctic and Arctic

1968 ◽  
Vol 46 (10) ◽  
pp. S823-S824
Author(s):  
S. N. Vernov ◽  
A. N. Charakhchyan ◽  
T. N. Charakhchyan ◽  
Yu. J. Stozhkov
Keyword(s):  
Cosmic Rays ◽  
Temperature Effects ◽  
Cosmic Ray ◽  
Primary Component ◽  
Low Energy ◽  
Cosmic Ray Intensity ◽  
Simultaneous Measurements ◽  
Murmansk Region ◽  
The Antarctic

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.

Are Anomalous Cosmic Rays the Main Contribution to the Low-Energy Galactic Cosmic Ray Spectrum?

2008 ◽  
Vol 680 (2) ◽  
pp. L105-L108 ◽  
Author(s):  
K. Scherer ◽  
H. Fichtner ◽  
S. E. S. Ferreira ◽  
I. Büsching ◽  
M. S. Potgieter
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Low Energy ◽  
Anomalous Cosmic Rays ◽  
Galactic Cosmic Ray

scholarly journals Time dependence of the helium flux measured by PAMELA

2019 ◽  
Vol 209 ◽  
pp. 01004
Author(s):  
N. Marcelli ◽  
O. Adriani ◽  
G. C. Barbarino ◽  
G. A. Bazilevskaya ◽  
R. Bellotti ◽  
...  
Keyword(s):  
Energy Range ◽  
Time Dependence ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Space Experiment ◽  
Precision Measurements ◽  
Solar Modulation ◽  
Monthly Basis ◽  
The Galaxy ◽  
Crucial Information

Precision measurements of the Z = 2 component in cosmic radiation provide crucial information about the origin and propagation of the second most abundant cosmic ray species in the Galaxy (9% of the total). These measurements, acquired with the PAMELA space experiment orbiting Earth, allow to study solar modulation in details. Helium modulation is compared to the modulation of protons to study possible dependencies on charge and mass. The time dependence of helium fluxes on a monthly basis measured by PAMELA has been studied for the period between July 2006 to January 2016 in the energy range from 800 MeV/n to ~ 20 GeV/n.

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