Absolute low-latitude sea-level muon intensity at large zenith angle

1976 ◽  
Vol 13 (3) ◽  
pp. 566-570 ◽  
Author(s):  
Deba Prasad Bhattacharyya
2013 ◽  
Vol 28 (16) ◽  
pp. 1350071 ◽  
Author(s):  
HALIL ARSLAN ◽  
MEHMET BEKTASOGLU

The zenith angle dependence of cosmic muon flux at sea level in the western, eastern, southern and northern azimuths have been investigated separately for Calcutta, India and Melbourne, Australia for muon momenta up to ~500 GeV /c using Geant4 simulation package. These two locations were selected due to the fact that they significantly differ in geomagnetic cutoff rigidity. The exponent n, which is defined by the relation I(θ) = I(0°) cos nθ, was obtained for each azimuth in Calcutta and Melbourne. By acquiring an agreement between the simulation results and the experimental ones, the simulation study was extended for different azimuth angles and higher muon momenta. It was shown that the angular dependence of the cosmic muon intensity decreases with the increase of muon momentum at both locations. Moreover, the exponent becomes independent of both geomagnetic location and the azimuth angle for muons with momentum above 10 GeV /c, and it is nearly zero above 50 GeV /c. Therefore, it can be concluded that the cosmic muons with momenta between 50 GeV /c and ~500 GeV /c reach the sea level almost isotropically.


1978 ◽  
Vol 31 (5) ◽  
pp. 451 ◽  
Author(s):  
DP Bhattacharyya

A study is made of the influence of long-term solar modulation on the low energy sea level muon spectrum near the geomagnetic equator. Recent experimental data are compared with theoretical results calculated from the phenomenological model of Allkofer and Dau. It is suggested that the observed enhancement in the muon intensity is mainly due to a shift in the solar potential.


2019 ◽  
Author(s):  
Darko Zaric ◽  
Ievgen Vovk ◽  
Martin Will ◽  
Razmik Mirzoyan ◽  
Jürgen Besenrieder ◽  
...  

2019 ◽  
Author(s):  
Darko Zaric ◽  
Razmik Mirzoyan ◽  
Ievgen Vovk ◽  
Petar Temnikov ◽  
Michele Peresano ◽  
...  

2019 ◽  
Vol 37 (4) ◽  
pp. 747-761 ◽  
Author(s):  
Veronika Barta ◽  
Gabriella Sátori ◽  
Kitti Alexandra Berényi ◽  
Árpád Kis ◽  
Earle Williams

Abstract. We have investigated the solar flare effects on ionospheric absorption with the systematic analysis of ionograms measured at midlatitude and low-latitude ionosonde stations under different solar zenith angles. The lowest recorded ionosonde echo, the minimum frequency (fmin, a qualitative proxy for the “nondeviative” radio wave absorption occurring in the D-layer), and the dfmin parameter (difference between the value of the fmin and the mean fmin for reference days) have been considered. Data were provided by meridionally distributed ionosonde stations in Europe and South Africa during eight X- and M-class solar flares in solar cycle 23. Total and partial radio fade-out was experienced at every ionospheric station during intense solar flares (> M6). The duration of the total radio fade-out varied between 15 and 150 min and it was highly dependent on the solar zenith angle of the ionospheric stations. Furthermore, a solar-zenith-angle-dependent enhancement of the fmin (2–9 MHz) and dfmin (1–8 MHz) parameters was observed at almost every station. The fmin and dfmin parameters show an increasing trend with the enhancement of the X-ray flux. Based on our results, the dfmin parameter is a good qualitative measure for the relative variation of the “nondeviative” absorption, especially in the case of the less intense solar flares, which do not cause total radio fade-out in the ionosphere (class < M6).


1976 ◽  
Vol 54 (18) ◽  
pp. 1880-1883 ◽  
Author(s):  
Deba Prasad Bhattacharyya

The pion and kaon spectra in the top of the atmosphere have been derived from the satellite data of cosmic ray nucleons by using the Bose-type distribution of secondary mesons produced in the inclusive reactions p + p → π− + X and p + p → K− + X. The derived pion and kaon spectra follow the relations of the form π(Eπ) dEπ = 0.184Eπ−2.6 dEπ and K(Ek) dEk = 0.036 Ek−2.6 dEk. With the help of the diffusion equation for pions and kaons in the atmosphere, the sea level muon spectrum has been derived and the results have been compared with the magnetic spectrograph data of Allkofer, Carstensen, and Dau in the muon momentum range 15–1000 GeV/c. The sea level muon intensity arising from kaon parentage increases with energy.


2014 ◽  
Vol 119 (8) ◽  
pp. 6865-6875 ◽  
Author(s):  
Neil R. Thomson ◽  
Mark A. Clilverd ◽  
Craig J. Rodger

1987 ◽  
Vol 24 (10) ◽  
pp. 1927-1951 ◽  
Author(s):  
Ian Knight ◽  
Noel P. James

The St. George Group is a ~500 m thick sequence of carbonate rock that accumulated during Early and early Middle Ordovician time in a series of shallow subtidal and peritidal environments near the outer edge of a low-latitude continental margin. Lithological variations, in the form of two megacycles, reflect deposition in response to eustatic fluctuations in sea level preceding and during the early stages of Taconic orogenesis.Strata are grouped into four formations of roughly equal thickness. The newly named basal Watts Bight Formation is a lower sequence of peritidal limestones and dolostones and an upper thicker, commonly dolomitized succession of burrowed carbonates distinguished by large digitate thrombolite mounds. The overlying Boat Harbour Formation (new) is a series of muddy, peritidal, shallowing-upward sequences of limestone and dolostone. A widespread subaerial disconformity near the top of the formation, reflecting eustaic sea-level fall and the end of the first megacycle, is marked by breccia, quartz-pebble conglomerate, paleokarst, and (or) extensive dolomitization and is succeeded by higher energy peritidal limestones called the Barbace Cove Member (new). The succeeding, thick, monotonous Catoche Formation (revised) is a succession of fossiliferous subtidal limestones with scattered thrombolite mounds whose upper part is locally affected by extensive, multigeneration dolomitization and Pb–Zn mineralization. The St. George Group is capped by the newly defined Aguathuna Formation, a stack of peritidal dolostones and minor limestones and shales deposited during a period of repeated exposure and synsedimentary faulting. An erosional disconformity, resulting from regional compressional tectonics and eustatic sea-level fall, locally marks the top of the St. George and the second megacycle.


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