On the nature of some anomalies in the cosmic-ray distribution

1968 ◽  
Vol 46 (10) ◽  
pp. S614-S616 ◽  
Author(s):  
N. P. Chirkov ◽  
G. F. Krymsky ◽  
A. I. Kuzmin
Keyword(s):  
Magnetic Field ◽  
Diurnal Variation ◽  
Interplanetary Magnetic Field ◽  
Equatorial Plane ◽  
Geomagnetic Field ◽  
Cosmic Ray ◽  
Neutron Monitors ◽  
Vector Method ◽  
Worldwide Network ◽  
Northern And Southern Hemispheres

Diurnal and semidiurnal variations of the data from the worldwide network of neutron monitors during 1958 are analyzed using the receiving-vector method. It is shown that there exists an "antisymmetric" diurnal variation, i.e., a variation with opposite phases in the northern and southern hemispheres. After correction for the distortion due to the geomagnetic field, it is found that this variation has an amplitude of 0.03% and an hour of maximum at 21.5 hours in the northern hemisphere. If the variation is due to cosmic-ray screening in the interplanetary magnetic field, this field must have a slope of 7° with respect to the solar equatorial plane.

scholarly journals On the character of cosmic ray variations at f>2x10<SUP>-5</SUP> Hz

1996 ◽  
Vol 3 (2) ◽  
pp. 135-141 ◽  
Author(s):  
K. Kudela ◽  
E. O. Flückiger ◽  
J. Torsti ◽  
H. Debrunner
Keyword(s):  
Magnetic Field ◽  
Time Series ◽  
Diurnal Variation ◽  
White Noise ◽  
Interplanetary Magnetic Field ◽  
Time Scales ◽  
Cosmic Ray ◽  
Neutron Monitors ◽  
Scaling Properties ◽  
Interplanetary Disturbance

Abstract. We examine the time series of cosmic ray (CR) intensity recorded by two neutron monitors (NMs) at medium latitudes for scaling properties on time scales shorter than the diurnal variation. Scaling of the data with 10 sec as well as I min resolution is shown to be complicated, indicating that there is probably not a unique process governing the CR fluctuations in the whole interval studied. For T < 20 min the general characteristics are similar to those of white noise. Above 40-60 min the scaling characteristics are dependent on the level of interplanetary disturbance. This is consistent with the concept of scattering CRs by inhomogeneities of the interplanetary magnetic field (IMF). With increasing interplanetary turbulence the dimensionality of the CR time series decreases. The region of stable scaling is, however, narrow, only up to 6 hours. Multifractality signatures in the region 1-6 hours are similar to those in the IMF, however the deviations from monofractality are relatively small.

The second spherical harmonic of the diurnal variation and the orientation of the interplanetary magnetic field

1968 ◽  
Vol 46 (10) ◽  
pp. S973-S975 ◽  
Author(s):  
G. V. Skeipin ◽  
P. A. Krivoshapkin ◽  
G. F. Krymsky ◽  
A. I. Kuzmin
Keyword(s):  
Magnetic Field ◽  
Diurnal Variation ◽  
Interplanetary Magnetic Field ◽  
Neutron Monitor ◽  
Spherical Harmonic ◽  
Cosmic Ray ◽  
Vector Information ◽  
Neutron Monitor Data ◽  
Distribution Vector ◽  
Monitor Data

The super neutron monitor data from Goose Bay and Deep River for 1965 have been analyzed to give month-to-month changes of the first and second harmonics of the solar-diurnal variation. Using these results together with various suppositions about the nature of the cosmic-ray distribution vector, information is obtained concerning the orientation of the interplanetary magnetic field.

Interplanetary magnetic field fluctuations and the diurnal variation of cosmic ray intensity

1975 ◽  
Vol 2 (12) ◽  
pp. 571-574 ◽  
Author(s):  
J. W. Sari ◽  
L. J. Lanzerotti ◽  
C. G. Maclennan ◽  
D. Venkatesan
Keyword(s):  
Magnetic Field ◽  
Diurnal Variation ◽  
Interplanetary Magnetic Field ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Field Fluctuations

Gradient of galactic cosmic rays normal to the solar equatorial plane

1968 ◽  
Vol 46 (10) ◽  
pp. S981-S984 ◽  
Author(s):  
D. Patel ◽  
V. Sababhai ◽  
G. Subramanian
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Rays ◽  
Interplanetary Magnetic Field ◽  
Equatorial Plane ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Cosmic Ray Intensity ◽  
Positive Exponent ◽  
Ray Density

Predictions concerning the anisotropy of galactic cosmic rays due to a gradient of cosmic-ray density perpendicular to the solar equatorial plane have been verified experimentally as follows. (1) The energy spectrum of the variation of the semidiurnal component has a positive exponent. (2) The diurnal and the semidiurnal components are oriented with respect to the interplanetary magnetic field. (3) A deficiency of cosmic-ray intensity, Tmin, is observed along the direction of the interplanetary magnetic field on days when the energy spectrum of the diurnal variation has an exponent different from zero.

USE OF COSMIC RAY MEASUREMENTS TO IDENTIFY THE SECTOR POLARITIES OF THE INTERPLANETARY MAGNETIC FIELD

2005 ◽  
Vol 20 (29) ◽  
pp. 6708-6710
Author(s):  
MONICA LAURENZA ◽  
MARISA STORINI ◽  
GIOVANNI MORENO
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Field ◽  
Cosmic Ray ◽  
Time Variability ◽  
Muon Component ◽  
The Antarctic ◽  
Wavelet Technique

The knowledge of the interplanetary magnetic field sector polarity at the Earth's location is relevant to study many phenomena related to the Space Climatology. We filled the gaps in the daily polarities of the interplanetary magnetic field derived from spacecraft observations by using two sets of ground-based measurements: i) the cosmic ray muon component intensities supplied by the multidirectional Nagoya telescope; ii) the geomagnetic field from the Antarctic Vostok Observatory. We discuss the time variability of the sector polarities inferred from the wavelet technique in the period 1971–1992.

scholarly journals Evaluation of the Interplanetary Magnetic Field Strength Using the Cosmic-Ray Shadow of the Sun

2018 ◽  
Vol 120 (3) ◽  
Author(s):  
M. Amenomori ◽  
X. J. Bi ◽  
D. Chen ◽  
T. L. Chen ◽  
W. Y. Chen ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Interplanetary Magnetic Field ◽  
Magnetic Field Strength ◽  
Cosmic Ray ◽  
The Sun
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