Investigation of the cosmic-ray east–west asymmetry

1968 ◽  
Vol 46 (10) ◽  
pp. S805-S808 ◽  
Author(s):  
E. A. Bogomolov ◽  
V. K. Karakadko ◽  
N. D. Lubyanaya ◽  
V. A. Romanov ◽  
M. G. Totubalina ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Zenith Angle ◽  
Cosmic Radiation ◽  
Flux Ratio ◽  
Cosmic Ray ◽  
Cerenkov Counter ◽  
Cerenkov Detector ◽  
Middle Latitudes ◽  
Primary Cosmic Radiation ◽  
East West

The east–west asymmetry has been measured to obtain a more accurate value of the antiproton–proton flux ratio in the primary cosmic radiation. The measurements have been carried out at middle latitudes at a depth of 10 g/cm2 of atmosphere and at a zenith angle of 60°. The telescope used for detection consisted of two scintillation counters, a lucite Cerenkov counter, and a gas Cerenkov counter. The threshold of the gas Cerenkov detector has been changed from 1.7 BeV to 5.2 BeV (for protons) in flight. For orientation of the device in space the earth's magnetic field was used.The preliminary results of the experiment are given.

Time variations of directional cosmic ray intensity at low latitude - II. Time variations of east-west asymmetry

1961 ◽  
Vol 263 (1312) ◽  
pp. 118-126 ◽  
Keyword(s):  
Geomagnetic Storms ◽  
Daily Variation ◽  
Cosmic Ray ◽  
Middle Latitude ◽  
Geomagnetic Disturbance ◽  
Equatorial Station ◽  
Cosmic Ray Intensity ◽  
Primary Cosmic Radiation ◽  
Time Variations ◽  
East West

Changes of the energy spectrum of primary cosmic radiation can be followed through the time variations of east-west asymmetry of the μ -meson component at low latitudes. Such a study has been conducted for the first time at Ahmedabad during 1957-8. The changes of east-west asymmetry are associated with changes of the daily variation of cosmic ray in­tensity, of the daily mean neutron intensity measured at equatorial and middle latitude stations, of the index of geomagnetic disturbance and of the horizontal component of the earth’s magnetic field. The study indicates that days with high east-west asymmetry are associated with geomagnetically quiet days and a cosmic ray daily variation consistent with its being produced by an anisotropy of primary radiation outside the influence of the geomagnetic field. On such days, the daily variation produced by the anisotropy, as observed at an equatorial station, has a significant diurnal as well as a semi-diurnal component. High east-west asymmetry and associated anisotropy occur 3 to 5 days before the arrival of solar corpuscular beams which envelop the earth. Days with low east-west asymmetry occur about 3 to 4 days after the onset of cosmic ray storms associated with geomagnetic storms, usually of the SC type.

A critical examination of the gravitational theory of the origin of cosmic rays

1950 ◽  
Vol 204 (1077) ◽  
pp. 278-294 ◽  
Keyword(s):  
Observational Data ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Present Theory ◽  
Gravitational Theory ◽  
Critical Examination ◽  
Gravitational Acceleration ◽  
Primary Cosmic Radiation ◽  
Order Of Magnitude ◽  
Intergalactic Space

The observational data which any theory of the origin of primary cosmic radiation should explain and the comparative merits of the various theories so far propounded are examined. In particular, Milne’s suggestion concerning a possible gravitational acceleration in intergalactic space is considered in detail, and his somewhat involved analysis is replaced by a simpler method of derivation by means of an alternative time-scale. The energy spectrum and possible total intensity of gravitationally accelerated material are examined; it is shown that an expression can be obtained for the former which is consistent with cosmic-ray data, but because the world-model considered is not sufficiently sharply defined, no order of magnitude can be obtained for the latter. It thus appears that a gravitational theory of cosmic radiation can account for most of the main features of the observational data, and as regards the remaining features, although the present theory is incomplete, it presents no actual inconsistencies with observation.

scholarly journals 39. The anisotropy of primary cosmic radiation and the electromagnetic state in interplanetary space

1958 ◽  
Vol 6 ◽  
pp. 377-385
Author(s):  
V. Sarabhai ◽  
N. W. Nerurkar ◽  
S. P. Duggal ◽  
T. S. G. Sastry
Keyword(s):  
Experimental Data ◽  
Cosmic Rays ◽  
Cosmic Radiation ◽  
Interplanetary Space ◽  
Daily Variation ◽  
Cosmic Ray ◽  
The Sun ◽  
Cosmic Ray Intensity ◽  
Daily Variations ◽  
Primary Cosmic Radiation

Study of the anisotropy of cosmic rays from the measurement of the daily variation of meson intensity has demonstrated that there are significant day-today changes in the anisotropy of the radiation. New experimental data pertaining to these changes and their solar and terrestrial relationships are discussed.An interpretation of these changes of anisotropy in terms of the modulation of cosmic rays by streams of matter emitted by the sun is given. In particular, an explanation for the existence of the recently discovered types of daily variations exhibiting day and night maxima respectively, can be found by an extension of some ideas of Alfvén, Nagashima, and Davies. An integrated attempt is made to interpret the known features of the variation of cosmic ray intensity in conformity with ideas developed above.

scholarly journals First analysis of inclined air showers detected by Tunka-Rex

2019 ◽  
Vol 216 ◽  
pp. 02012
Author(s):  
T. Marshalkina ◽  
P.A. Bezyazeekov ◽  
N.M. Budnev ◽  
D. Chernykh ◽  
O. Fedorov ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Radio Emission ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Air Showers ◽  
Standard Analysis ◽  
Air Shower ◽  
The Magnetic Field

The Tunka Radio Extension (Tunka-Rex) is a digital antenna array for the detection of radio emission from cosmic-ray air showers in the frequency band of 30 to 80 MHz and for primary energies above 100 PeV. The standard analysis of Tunka-Rex includes events with zenith angle of up to 50?. This cut is determined by the efficiency of the external trigger. However, due to the air-shower footprint increasing with zenith angle and due to the more efficient generation of radio emission (the magnetic field in the Tunka valley is almost vertical), there are a number of ultra-high-energy inclined events detected by Tunka-Rex. In this work we present a first analysis of a subset of inclined events detected by Tunka-Rex. We estimate the energies of the selected events and test the efficiency of Tunka-Rex antennas for detection of inclined air showers.

Recent Evidence Concerning the Sidereal Anisotropy in the Charged Primary Cosmic Radiation

1969 ◽  
Vol 1 (6) ◽  
pp. 278-280 ◽  
Author(s):  
K. G. Jacklyn ◽  
A. Vrana
Keyword(s):  
Magnetic Field ◽  
Pitch Angle ◽  
Cosmic Radiation ◽  
Particle Trajectory ◽  
Magnetic Moments ◽  
Charged Particles ◽  
Significant Evidence ◽  
Primary Cosmic Radiation ◽  
The Magnetic Field ◽  
Sidereal Anisotropy

Significant evidence for a bi-directional sidereal anisotropy has been obtained from observations with meson telescopes at depths in the vicinity of 40 metres water equivalent (m.w.e.) underground. The anisotropy is of the type which should occur when charged particles which were formerly isotropic stream equally in both directions along a magnetic field, if there is a tendency for pitch angles to become reduced (the pitch angle being the angle between the particle trajectory and the direction of the field). If the magnetic moments of the particles are adiabatically invariant, changes in the magnetic field, both with position and time, could be responsible for the anisotropy.

The long-term variation of the cosmic radiation

1968 ◽  
Vol 46 (10) ◽  
pp. S903-S906 ◽  
Author(s):  
J. A. Lockwood ◽  
W. R. Webber
Keyword(s):  
Neutron Monitor ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Solar Modulation ◽  
Neutron Monitors ◽  
Cosmic Ray Intensity ◽  
Direct Measurements ◽  
Term Variation ◽  
Primary Cosmic Radiation

The variation in the cosmic-ray intensity recorded by neutron monitors from 1958 to 1965 has been investigated to deduce the form of the solar modulation of the cosmic radiation. The observed changes in the intensity at the neutron monitor stations, averaged over quarter-year periods, were compared with changes calculated using modulation functions depending upon energy, rigidity, and velocity × rigidity. These calculations were based upon the revised differential response functions deduced by Lockwood and Webber (1967). The variance between the observed and calculated changes in the neutron monitor intensities at different stations was minimized to determine the best form of the solar modulation function. We find that the change of the primary cosmic radiation, deduced from the change in the neutron monitor intensity as well as from direct measurements of the primary flux, can be described by a modulation of the form exp(–K/P) in the rigidity range 0.5 < P < 50 GV. The change between 1959 and 1965 can be fitted with K = 1.94 ± 0.09 and between 1963 and 1965 with K = 0.36 ± 0.05.

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.

Rigidity spectra of primary cosmic radiation

1968 ◽  
Vol 46 (10) ◽  
pp. S923-S926
Author(s):  
K. Kasturirangan ◽  
N. W. Nerurkar
Keyword(s):  
Solar Activity ◽  
North America ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Slow Change ◽  
Primary Cosmic Radiation ◽  
Ion Chambers

The comparison of the cosmic-ray intensity measured with balloon-borne ion chambers at different atmospheric depths at stations in North America and in the U.S.S.R. for the period 1937–67 is presented. It is found that there is no difference in variations of cosmic-ray spectra in periods of increasing and decreasing solar activity in 1954–64. In 1937–40 the cosmic-ray spectra are found to be distinctly different, suggesting a slow change in the spectrum over periods greater than the 11-year cycle of solar activity.

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