Cosmic rays and particle physics

By Thomas K. Gaisser. 2016

819 citations recorded by the source corpus.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/dc3bf5bd1c17297455d4821e81826a497f342f56

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In Nuclear and High Energy Physics

Citations in the corpus

A COMBINED MAXIMUM-LIKELIHOOD ANALYSIS OF THE HIGH-ENERGY ASTROPHYSICAL NEUTRINO FLUX MEASURED WITH ICECUBE (2015, methodology): “decay, the resulting neutrino flux differs from the original cosmic ray flux in its energy and zenith angle dependence: the energy spectrum is steeper (approximately E) and the flux is enhanced toward the horizon (Gaisser 1990).”
A Study of the Composition of Ultra-High-Energy Cosmic Rays Using the High-Resolution Fly’s Eye (2002, background): “The general dependence of Xmax on energy can be seen in a simple branching model in which Nmax / E0 and Xmax / ln E0 (Gaisser 1990; Heitler 1944).”
Neutrino flux prediction at MiniBooNE (2008, background): “e take ˘(t) ’˘(0) = 0:19 [16]. Concerning electron (anti-)neutrinos from decays, we neglect terms proportional to the electron mass and assume the following neutrino energy and angular distribution [17]: dN dxd = 12x2 4ˇ (1 x)[1 P zcos( )] (7) where cos( ) is the neutrino emission angle with respe”
Energetic Particle Influence on the Earth’s Atmosphere (2015, background): “In more detail CR composition and energy spectra are considered in the works of Simpson (1983) and Gaisser (1990).”
Geophysical muon imaging: feasibility and limits (2010, methodology): “…O N The interest in using muon imaging for Earth Sciences purposes soon arose after the discovery of cosmic rays (Auger 1941; Leprince-Ringuet 1945; Gaisser 1990; Crozon 2005) and muons (Neddermeyer & Anderson 1937, 1938), when it was realised that muons of cosmic origin are able to cross hundred…”
Cosmogenic nuclide systematics and the CRONUScalc program (2016, background): “Unlike the hadronic component of the flux, the muonic 1251 flux increases and then reaches a plateau as the cascade moves down through 1252 the atmosphere because muons do not interact as strongly as neutrons and 1253 are lost very slowly through ionization (Gaisser, 1990).”
Cosmic-Ray Electrons in Groups and Clusters of Galaxies: Primary and Secondary Populations from a Numerical Cosmological Simulation (2001, background): “Production of Secondary Electrons The main channels for the production of secondary elec- trons are given by (Gaisser 1990) p ] p ] nB ] X , (2) p ] p ] KB] X , (3) where X indicates all the other by-products of the reactions.”
The EXO-200 detector, part I: detector design and construction (2012, methodology): “gated using the GEANT 3.21 detector simulation. Muons were generated with a ratio of m+=m of 1.25. The muon energy spectrum was parameterized in varying degrees of detail using equations from Gaisser [69]. Ultimately, the following form was used: dN dE µE (g+1) 0 1 1+1:1E 0=(115GeV) + 0:054 1+1:1E ”
Synchrotron Self-Compton Analysis of TeV X-Ray-Selected BL Lacertae Objects (2008, background): “The particle acceleration timescale in the comoving frame for a Fermi mechanism is t′acc = Na γ′ νB (52) where Na & 1 is the number of gyrations an electron makes while doubling its energy, and νB = eB 2πmec is the Larmor frequency (e.g., Gaisser 1990).”
The Large Hadron-Electron Collider at the HL-LHC (2020, background): “They emerge as decay products of pions, kaons and charmed mesons, and possibly beauty mesons if the energy is high enough [307].”