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.

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 Latitudinal and radial variation of >2 GeV/n protons and alpha-particles at solar maximum: ULYSSES COSPIN/KET and neutron monitor network observations

2003 ◽  
Vol 21 (6) ◽  
pp. 1295-1302 ◽  
Author(s):  
A. V. Belov ◽  
E. A. Eroshenko ◽  
B. Heber ◽  
V. G. Yanke ◽  
A. Raviart ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Neutron Monitor ◽  
Solar Minimum ◽  
Latitudinal Gradient ◽  
Solar Maximum ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Alpha Particles ◽  
Polar Regions

Abstract. Ulysses, launched in October 1990, began its second out-of-ecliptic orbit in September 1997. In 2000/2001 the spacecraft passed from the south to the north polar regions of the Sun in the inner heliosphere. In contrast to the first rapid pole to pole passage in 1994/1995 close to solar minimum, Ulysses experiences now solar maximum conditions. The Kiel Electron Telescope (KET) measures also protons and alpha-particles in the energy range from 5 MeV/n to >2 GeV/n. To derive radial and latitudinal gradients for >2 GeV/n protons and alpha-particles, data from the Chicago instrument on board IMP-8 and the neutron monitor network have been used to determine the corresponding time profiles at Earth. We obtain a spatial distribution at solar maximum which differs greatly from the solar minimum distribution. A steady-state approximation, which was characterized by a small radial and significant latitudinal gradient at solar minimum, was interchanged with a highly variable one with a large radial and a small – consistent with zero – latitudinal gradient. A significant deviation from a spherically symmetric cosmic ray distribution following the reversal of the solar magnetic field in 2000/2001 has not been observed yet. A small deviation has only been observed at northern polar regions, showing an excess of particles instead of the expected depression. This indicates that the reconfiguration of the heliospheric magnetic field, caused by the reappearance of the northern polar coronal hole, starts dominating the modulation of galactic cosmic rays already at solar maximum.Key words. Interplanetary physics (cosmic rays; energetic particles) – Space plasma physics (charged particle motion and acceleration)

Energy spectra of carbon and oxygen - Predictions from HELIOS E6 for Solar Orbiter HET

2020 ◽  
Author(s):  
Johannes Marquardt ◽  
Bernd Heber ◽  
Robert Elftmann ◽  
Robert Wimmer-Schweingruber
Keyword(s):  
Energetic Particle ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
High Energy ◽  
Energy Spectra ◽  
Particle Detector ◽  
Quiet Time ◽  
Transport Models ◽  
Galactic Cosmic Ray ◽  
Insight Into

<p>Anomalous cosmic rays (ACRs) are well-suited to probe the transport conditions of energetic particles in the innermost heliosphere. We revisit the HELIOS Experiment 6 (E6) data in view of the upcoming Solar Orbiter Energetic Particle Detector (EPD) suite that will perform measurements during a comparable solar minimum within the same distance.</p><p>Adapting the HELIOS energy ranges for oxygen and carbon to the ones given by the High Energy Telescope (HET) allows us to determine predictions for the upcoming measurements but also to put constraints on particle transport models that provide new insight into the boundary conditions close to the Sun.</p><p>We present here the adapted energy spectra of galactic cosmic ray (GCR) carbon and oxygen, as well as of ACR oxygen during solar quiet time periods between 1975 to 1977. Due to the higher energy threshold of HET in comparison to E6 gradients of about 20% at 15 MeV/nucleon are expected. The largest ACR gradient measured by E6 was obtained to be about 75% between 9 and 13 MeV/nucleon and 0.4 AU and 1 AU.</p>

The Propagation of Cosmic Radiation Through the Inter-Planetary Magnetic Field

1967 ◽  
Vol 1 (1) ◽  
pp. 29-30
Author(s):  
K. G. McCracken
Keyword(s):  
Magnetic Field ◽  
Energy Range ◽  
Cosmic Radiation ◽  
Counting Rate ◽  
Cosmic Ray ◽  
Alpha Particles ◽  
Statistical Precision ◽  
Degree Of Anisotropy ◽  
Planetary Magnetic Field ◽  
Cosmic Ray Flux

Instruments were flown on the Pioneer 6 and 7 spacecraft during 1965-66 to study the degree of anisotropy of cosmic radiation in the energy range 7.5-90 Mev/nucleón. The instruments record the cosmic ray fluxes from each of four contiguous ‘quadrants’ of azimuthal rotation of the spacecraft, for each of three energy windows 7.5-45 Mev, 45-90 Mev, and 150-350 Mev for alpha particles and heavier nuclei. In addition, the counting rate of all particles of energy >7.5 Mev is recorded, thereby providing cosmic ray data of high statistical precision useful in the study of fast changes in the cosmic ray flux.

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.

scholarly journals A united model for the cosmic ray energy spectra and anisotropy in the energy range 100 – 100 000 GeV

2013 ◽  
Vol 409 ◽  
pp. 012028 ◽  
Author(s):  
V I Zatsepin ◽  
A D Panov ◽  
N V Sokolskaya
Keyword(s):  
Energy Range ◽  
Cosmic Ray ◽  
Energy Spectra

scholarly journals FURTHER TEST MASS CHARGING SIMULATIONS FOR ASTROD I

2008 ◽  
Vol 17 (07) ◽  
pp. 965-983 ◽  
Author(s):  
GANG BAO ◽  
WEI-TOU NI ◽  
D. N. A. SHAUL ◽  
H. M. ARAUJO ◽  
LEI LIU ◽  
...  
Keyword(s):  
Solar Minimum ◽  
Cosmic Ray ◽  
Test Mass ◽  
Alpha Particles ◽  
Space Environment ◽  
Science Data ◽  
Charging Rate ◽  
Noise Limit ◽  
Galactic Cosmic Ray

The electrostatic test mass charging in the ASTROD I (Astrodynamical Space Test of Relativity using Optical Devices I) mission can affect the quality of the science data due to spurious Coulomb and Lorentz forces. To estimate the size of the resultant disturbances, credible predictions of charging rates and the charging noise are required. Using the GEANT4 software toolkit, we present a detailed Monte Carlo simulation of ASTROD I test mass charging due to exposure of the spacecraft to galactic cosmic-ray (GCR) protons and alpha particles (3 He , 4 He ) in the space environment. A positive charging rate of 33.3 e+/s at solar minimum is predicted. The predicted rate reduces by 50% at solar maximum. Based on this charging rate and factoring in the contribution of minor cosmic-ray components, we calculate the acceleration noise and stiffness associated with charging. We conclude that the acceleration noise arising from Coulomb and Lorentz effects are well below the ASTROD I acceleration noise limit at 0.1 mHz both at solar minimum and maximum. The magnitude of coherent Fourier components due to charging are also estimated.

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

Composition and energy spectra of cosmic-ray primaries in the energy range 1013–1015 eV/particle observed by Japanese–Russian joint balloon experiment

2001 ◽  
Vol 16 (1) ◽  
pp. 13-46 ◽  
Author(s):  
A.V. Apanasenko ◽  
V.A. Sukhadolskaya ◽  
V.A. Derbina ◽  
M. Fujii ◽  
V.I. Galkine ◽  
...  
Keyword(s):  
Energy Range ◽  
Cosmic Ray ◽  
Energy Spectra ◽  
Balloon Experiment
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