Cosmic Rays at Sea Level

A New Full 3‐D Model of Cosmogenic Tritium 3H Production in the Atmosphere (CRAC:3H)

“…The yield function should not be confused with the so‐called production function S i ( E , h ), which is defined as the number of nuclide atoms produced in the unit atmospheric layer per one incident particle with the energy E . In a case of the isotropic particle distribution, these quantities are related as where π is the conversion factor between the particle intensity in space and the particle flux at the top of the atmosphere (see, e.g., chapter 1.6.2 in Grieder, 2001).…”

Measurement and simulation of neutron monitor count rate dependence on surrounding structure

“…Furthermore, the effects of local surroundings and atmospheric structure require detailed study for each location. While much interesting science can be done without precise knowledge of the yield function [ Grieder , ], a neutron monitor will become a more powerful instrument when its yield function is fully understood and data from the worldwide network of neutron monitors can be combined to precisely track the GCR spectrum. Combining data from neutron monitors at various cutoff rigidities can also be useful in the analyses of relativistic solar particle events [ Cramp et al , ; Vashenyuk et al , ].…”

Performance of the Water Cherenkov detector LAGO-Chiapas, Mexico

“…The hadronic interaction models used at high and low energies were QGSJETII-4 and GHEISHA, respectively (see the CORSIKA manual for more details [2]). The distribution of primaries at the top of the atmosphere was calculated according to [3], taking into account the measured spectra for nuclei with atomic number within the range 1 ≤ Z ≤ 28 [4]. In Figure 2, we show the fluence at the detector level for the FCFM campus and in Figure 3 for the top of the Tacaná volcano site.…”