Cosmic rays and particle physics

By K. Kampert. 2001

1,029 citations recorded by the source corpus.

The study of high energy cosmic rays is a diversified field of observational and phenomenological physics addressing questions ranging from shock acceleration of charged particles in various astrophysical objects, via transport properties through galactic and extragalactic space, to questions of dark matter, and even to those of particle physics beyond the Standard Model including processes taking place in the earliest moments of our Universe. After decades of mostly independent evolution of nuclear, particle and high energy cosmic ray physics we find ourselves entering a symbiotic era of these fields of research. Some examples of interrelations will be given from the perspective of modern Particle-Astrophysics and new major experiments will briefly be sketched.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/aeb03081a55244b70bb54575bb1386b128e8edfe

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Citations in the corpus

The IceCube Neutrino Observatory - Contributions to ICRC 2015 Part II: Atmospheric and Astrophysical Diffuse Neutrino Searches of All Flavors (2015, background): “If the Fermi shock acceleration mechanism is responsible for the acceleration of the cosmic rays, a power law energy spectrum with spectral index close to −2 is expected [18].”
IceTop: The Surface Component of IceCube (2003, background): “For higher primary energies, the number of muons increases, and the multiplicity in showers generated by nuclei approaches asymptotically a factor of A times the muon multiplicity of a proton shower [58], yielding about 2.”
DarkSUSY: Computing Supersymmetric Dark Matter Properties Numerically (2004, methodology): “To model the propagation we have considered a semi-empirical diffusion equation [103, 104], in the steady state approximation, applied to a two-dimensional model with cylindrical symmetry and with free escape boundary conditions.”
Neutron Monitor Response Functions (2000, methodology): “14 km) concentric spherical shells with di ering radii and density to simulate the actual density pro le (Gaisser, 1990) with a vertical total 1033g/cm2 column density for sea level and 305 g/cm2 for 9.”
Energy spectra of gamma rays, electrons, and neutrinos produced at proton-proton interactions in the very high energy regime (2006, background): “[9]), the contribution through decays of other unstable secondaries, first of all K mesons, is not negligible.”
Prompt neutrino fluxes from atmospheric charm (2008, neutral): “[14, 15, 62, 63] for calculating the flux.”
Hadronic multiparticle production at ultrahigh energies and extensive air showers (2010, background): “It is assumed that a charged pion (π or π) of energy E interacts after one interaction length λI (≈ 120 g/cm 2 for pions of 10 − 1000GeV [60]) and produces r nmult charged pions and c nmult neutral pions, see Fig.”
Energy spectra of gamma-rays, electrons and neutrinos produced at interactions of relativistic protons with low energy radiation (2008, neutral): “[13]), the parameters in the Tables II calculated for e and ν̄μ for small η should be identical.”
QED cascades induced by circularly polarized laser fields (2010, methodology): “According to Monte-Carlo simulations [24], the resulting analytical approach works much worse here than in the case of 1D approximation for EAS.”
Cosmic neutrino pevatrons: A brand new pathway to astronomy, astrophysics, and particle physics (2013, background): “Many of the salient features of the two models can be visualized in terms of a “leaky box,” in which CRs propagate freely in the Galaxy, contained by the magnetic field but with some probability to escape which is constant in time [149].”
IceCube high-energy starting event sample: Description and flux characterization with 7.5 years of data (2020, background): “The observation of EeV cosmic rays indicates that objects of large size or high magnetic field strength are accelerating charged particles to high energies, narrowing the search for neutrino sources to a subclass of objects [14,15].”
Diffuse Neutrino Intensity from the Inner Jets of Active Galactic Nuclei: Impacts of External Photon Fields and the Blazar Sequence (2014, background): “The dependence E νLE′ ν ∝ E ′2 ν is suggested from the decay kinematics of charged pions [62].”
Ltd Registered in England and Wales Registered Number : 1072954 Registered office : (2004, background): “An excellent introduction to cosmic rays and their interactions may be found in [31].”
A facility to search for hidden particles at the CERN SPS: the SHiP physics case (2015, neutral): “decay distributions have simple forms [962].”
The Muon Puzzle in cosmic-ray induced air showers and its connection to the Large Hadron Collider (2021, background): “c rays, as discussed in Section2.1. The steep cosmic-ray spectrum emphasises the particle production phase space at x lab >0:1, and suppresses the importance of pion-air and kaon-air interactions (Gaisser et al. 2016;Fedynitch et al.2018b). If the muon decit in simulated air showers is caused by ”
High-energy neutrinos in the context of multimessenger astrophysics (2007, background): “The spectrum is one power steeper than the spectral behavior of the primaries, since the probability that pions and kaons interact before decaying increases with the energy [Gai90].”