Cosmic-ray isotopic composition of C, N, O, Ne, Mg, SI nuclei in the energy range 50-200 MeV per nucleon measured by the Voyager spacecraft during the solar minimum period

1994 ◽  
Vol 426 ◽  
pp. 366 ◽  
Author(s):  
A. Lukasiak ◽  
P. Ferrando ◽  
F. B. McDonald ◽  
W. R. Webber
Keyword(s):  
Isotopic Composition ◽  
Energy Range ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
Minimum Period

Studies of the cosmic ray radial and latitudinal intensity gradients over the cycle 22 solar minimum period

1999 ◽  
Vol 23 (3) ◽  
pp. 453-458 ◽  
Author(s):  
F.B McDonald ◽  
Z Fujii ◽  
P Ferrando ◽  
B Heber ◽  
A Raviart ◽  
...  
Keyword(s):  
Solar Minimum ◽  
Cosmic Ray ◽  
Minimum Period

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 Cosmic-ray observations in 1964–65 with Mariner IV

1968 ◽  
Vol 46 (10) ◽  
pp. S976-S980 ◽  
Author(s):  
S. M. Krimigis
Keyword(s):  
Energy Range ◽  
Solar Minimum ◽  
Interplanetary Medium ◽  
Cosmic Ray ◽  
University Of Iowa ◽  
The University

The University of Iowa equipment on Mariner IV, which was launched towards Mars on 28 November 1964, consists in part of two thin-window G-M tubes sensitive to electrons of [Formula: see text] (detector B) and [Formula: see text] (detector A), and a shielded G-M tube (detector C) sensitive to electrons of Ee > 150 keV and having a threshold of ~55 MeV for omnidirectional protons. Observations over the period 28 November 1964 to 30 September 1965 have shown the following: (a) Electrons in the energy range [Formula: see text] were present in the interplanetary medium prior to day 12, 1965 with intensities of ~0.5 (cm2 s sr)−1. (b) The interplanetary cosmic-ray gradient for protons of [Formula: see text] was less than 3% per AU and the data are consistent with zero gradient. (c) There are large changes in the intensities of protons of [Formula: see text], but the direction and magnitude of the gradient for such protons were uncertain during solar minimum. The implications of these results are discussed.

Primary protons and alpha particles in the energy range 70–240 MeV/nucleon observed during 1966

1968 ◽  
Vol 46 (10) ◽  
pp. S900-S902
Author(s):  
G. D. Badhwar ◽  
C. L. Deney ◽  
B. R. Dennis ◽  
M. F. Kaplon
Keyword(s):  
Energy Range ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
Alpha Particles ◽  
Energy Spectra ◽  
Modulation Function ◽  
Residual Material ◽  
Acceptance Range

The differential energy spectra of cosmic-ray protons and helium nuclei were measured on two balloon flights from Fort Churchill, Canada, during late July and early August of 1966. The measurements were made using a double dE/dx vs. E detector with an energy-independent (for stopping particles) acceptance aperture of 6 cm2 sr. The detector floated for a total of 25 hours under 2.7 g/cm2 of residual material. The acceptance range of energies is 70–240 MeV/nucleon for protons and 4He. Both the proton and 4He differential spectra are depressed from solar minimum and appear similar to 1963 results. The P/He ratio over the energy range is 4.3 ± 1. The spectra are compared to those obtained in 1965. It is found that the modulation function is proportional to either R or Rβ.

scholarly journals GALACTIC COSMIC-RAY ENERGY SPECTRA AND COMPOSITION DURING THE 2009-2010 SOLAR MINIMUM PERIOD

2013 ◽  
Vol 770 (2) ◽  
pp. 117 ◽  
Author(s):  
K. A. Lave ◽  
M. E. Wiedenbeck ◽  
W. R. Binns ◽  
E. R. Christian ◽  
A. C. Cummings ◽  
...  
Keyword(s):  
Solar Minimum ◽  
Cosmic Ray ◽  
Energy Spectra ◽  
Minimum Period ◽  
Galactic Cosmic Ray

Nucleosynthesis in Wolf-Rayet stars and galactic cosmic-ray isotopic composition

1984 ◽  
Vol 4 (2-3) ◽  
pp. 109-114 ◽  
Author(s):  
N. Prantzos
Keyword(s):  
Isotopic Composition ◽  
Cosmic Ray ◽  
Galactic Cosmic Ray

scholarly journals Measurement of Low-Energy Cosmic-Ray Antiprotons at Solar Minimum

1998 ◽  
Vol 81 (19) ◽  
pp. 4052-4055 ◽  
Author(s):  
H. Matsunaga ◽  
S. Orito ◽  
H. Matsumoto ◽  
K. Yoshimura ◽  
A. Moiseev ◽  
...  
Keyword(s):  
Solar Minimum ◽  
Cosmic Ray ◽  
Low Energy

Isotopic composition of primary cosmic-ray nitrogen and oxygen with consequences for source models

1979 ◽  
Vol 63 (1) ◽  
pp. 215-236 ◽  
Author(s):  
L. Jacobsson ◽  
G. J�nsson ◽  
K. Kristiansson
Keyword(s):  
Isotopic Composition ◽  
Cosmic Ray ◽  
Source Models
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