World-wide cosmic-ray variations, 1937‐1952

1993 ◽  
pp. 183-200
Author(s):  
Scott E. Forbush
Keyword(s):  
World Wide ◽  
Cosmic Ray

World-Wide Changes in Cosmic-Ray Intensity

1939 ◽  
Vol 11 (3-4) ◽  
pp. 168-172 ◽  
Author(s):  
S. E. Forbush
Keyword(s):  
World Wide ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

On World-Wide Changes in Cosmic-Ray Intensity

1938 ◽  
Vol 54 (12) ◽  
pp. 975-988 ◽  
Author(s):  
S. E. Forbush
Keyword(s):  
World Wide ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

World-wide Effect in Cosmic Ray Intensity, as Observed during a Recent Magnetic Storm

Nature ◽  
1937 ◽  
Vol 140 (3538) ◽  
pp. 316-317 ◽  
Author(s):  
VICTOR F. HESS ◽  
A. DEMMELMAIR
Keyword(s):  
Magnetic Storm ◽  
World Wide ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

World-Wide Changes in the Phase of the Cosmic-Ray Solar Daily Variation

Nature ◽  
1953 ◽  
Vol 171 (4360) ◽  
pp. 918-920 ◽  
Author(s):  
T. THAMBYAHPILLAI ◽  
H. ELLIOT
Keyword(s):  
World Wide ◽  
Daily Variation ◽  
Cosmic Ray ◽  
Solar Daily Variation

A WORLD-WIDE STUDY OF THE DAILY VARIATION OF THE NUCLEONIC COMPONENT OF COSMIC RAYS

1960 ◽  
Vol 38 (8) ◽  
pp. 1011-1026 ◽  
Author(s):  
J. Katzman ◽  
D. Venkatesan
Keyword(s):  
Diurnal Variation ◽  
Phase Angle ◽  
World Wide ◽  
Pressure Effect ◽  
Cosmic Ray ◽  
Mean Amplitude ◽  
Short Term ◽  
Nucleonic Component ◽  
The Mean ◽  
Considerable Spread

The semidiurnal component of the nucleonic intensity at Ottawa, Canada, is essentially a pressure effect for the 5-year period, 1955 to 1959. The diurnal variation is composed of the component due to pressure, and a component that may be attributed to an anisotropy of the primary cosmic-ray particles. The results are confirmed by a comparative study of the data from 15 stations between the geomagnetic latitudes 83 °N. and 73 °S.A world-wide barometric coefficient of −0.72% per mb was obtained from the semidiurnal component and this coefficient was used to correct the diurnal component at all the stations. The average corrected diurnal variation during the period of study common to all stations, August 1957 to October 1958, is 0.27% and occurs at 14 h 16 m solar time. There is considerable spread in both amplitude and phase angle amongst the various stations. The root mean square differences from the mean amplitude is ±0.05% and from the mean phase angle is ±10° (40 minutes in time). The difficulty of drawing definite conclusions about the anisotropy from short-term studies of individual stations is pointed out.

NEW NEUTRON MONITOR STATION IN BAKSAN VALLEY

2005 ◽  
Vol 20 (29) ◽  
pp. 6696-6698 ◽  
Author(s):  
S. N. KARPOV ◽  
Z. M. KARPOVA ◽  
V. B. PETKOV ◽  
E. V. VASHENYUK ◽  
V. G. YANKE
Keyword(s):  
Solar Activity ◽  
High Altitude ◽  
Neutron Monitor ◽  
World Wide ◽  
Cosmic Ray ◽  
Northern Caucasus ◽  
Forbush Decreases ◽  
Monitor Station ◽  
The World

In autumn 2003 a new high-altitude neutron monitor (NM) station located in the Baksan Valley of Northern Caucasus was included in the world-wide network of NMs. The Baksan NM has already registered powerful cosmic ray variations (Forbush–decreases) connected with solar activity in October–November 2003. Since February 2004 the Baksan NM data are accessible via Internet: 〈〉

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