Nuclear composition of 1-to 20-PeV primary cosmic rays according to lateral features of the electron-photon component of all extensive air showers and of extensive air showers accompanying high-energy gamma rays and hadrons in x-ray emulsion chambers at the Tien Shan level

2003 ◽  
Vol 66 (5) ◽  
pp. 847-853
Author(s):  
N. M. Nesterova ◽  
V. P. Pavlyuchenko ◽  
A. P. Chubenko ◽  
S. B. Shaulov
1968 ◽  
Vol 46 (10) ◽  
pp. S131-S135 ◽  
Author(s):  
B. K. Chatterjee ◽  
N. V. Gopalakrishnan ◽  
G. T. Murthy ◽  
S. Naranan ◽  
B. V. Sreekantan ◽  
...  

The following results on the low-energy (> 0.6 GeV and > 1.0 GeV) muons in air showers of size 105 to 2 × 107 at Ootacamund (800 g cm−2) are obtained: (1) The average total number of muons [Formula: see text] varies as Ne0.32 ± 0.2 for 105 < Ne < 106, and as Ne0.8 ± 0.15for 106 < Ne < 2 × 107. (2) In showers showing flat electron lateral structure, the [Formula: see text] variation with Ne is similar to (1). However, in steep showers, [Formula: see text] varies as Ne0.75 ± 0.15 in the whole size range 105 to 2 × 107. (3) "Muon-rich" showers of size < 106 have less energy in the electron–photon component compared to "normal" showers. No such difference is found for showers of size > 106. (4) There is a slight indication of a deficiency of muon-rich showers having a flat lateral distribution of electrons in the right ascension interval 15–21 hours for showers of size 106–107. A similar deficit of showers was observed by the Tokyo group for muon-rich showers in the same RA interval.


1990 ◽  
Vol 16 (12) ◽  
pp. 1773-1803 ◽  
Author(s):  
P M Chadwick ◽  
T J L McComb ◽  
K E Turver

2007 ◽  
Author(s):  
X. Y. Wang ◽  
Z. Li ◽  
P. Mészáros

2003 ◽  
Vol 599 (2) ◽  
pp. 909-917 ◽  
Author(s):  
I. de la Calle Perez ◽  
I. H. Bond ◽  
P. J. Boyle ◽  
S. M. Bradbury ◽  
J. H. Buckley ◽  
...  

1958 ◽  
Vol 3 (32) ◽  
pp. 826-830 ◽  
Author(s):  
N. A. Porter ◽  
T. E. Cranshaw ◽  
J. F. De Beer ◽  
A. G. Parham ◽  
A. C. Sherwood

1998 ◽  
Vol 188 ◽  
pp. 459-460
Author(s):  
R. Shibata ◽  
T. Murakami ◽  
Y. Ueda ◽  
A. Yoshida ◽  
F. Tokanai ◽  
...  

We made a search of quiescent X-ray counterparts of two Gamma-Ray Bursts (GRBs), GRB930131 and GRB940217. These GRBs were detected with BATSE, EGRET, COMPTEL on board CGRO together with the GRB detector on Ulysses spacecraft, then they were localized in small error regions. These observations showed that the bursts were remarkably bright accompanying delayed high energy gamma-rays. ASCA observations have found a single X-ray source for each GRB on the possible location determined with the above instruments.


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