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Journal articles on the topic 'Cosmic-ray theory'

Author: Grafiati

Published: 14 March 2023

Last updated: 31 July 2025

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1

Hand, Eric. "Cosmic-ray theory unravels." Nature 463, no. 7284 (2010): 1011. http://dx.doi.org/10.1038/4631011a.

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Ferreira, Stefan E. S. "Theory of cosmic ray modulation." Proceedings of the International Astronomical Union 4, S257 (2008): 429–38. http://dx.doi.org/10.1017/s1743921309029664.

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AbstractThis work aims to give a brief overview on the topic of cosmic ray modulation in the heliosphere. The heliosphere, heliospheric magnetic field, transport parameters and the transport equation together with modulation models, which solve this equation in various degree of complexity, are briefly discussed. Results from these models are then presented where first it is shown how cosmic rays are globally distributed in an asymmetrical heliosphere which results from the relative motion between the local interstellar medium and the Sun. Next the focus shifts to low-energy Jovian electrons.

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3

Dorman, L. I., and I. V. Dorman. "Cosmic-ray atmospheric electric field effects." Canadian Journal of Physics 73, no. 7-8 (1995): 440–43. http://dx.doi.org/10.1139/p95-063.

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Experimental data on the atmospheric electric field effect in the cosmic-ray muon component are discussed on the basis of the general theory of cosmic-ray meteorological effects. In this framework, we develop the theory of atmospheric electric field effects in the hard- and soft-muons of secondary cosmic rays and in the neutron-monitor counting rates as well. We show that the experimental results can be understood on the basis of this theory. We also show that a sufficient atmospheric electric field effect in the cosmic-ray neutron component is to be expected because the neutron monitors work

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4

Ivlev, Alexei V., Kedron Silsbee, Marco Padovani, and Daniele Galli. "Rigorous Theory for Secondary Cosmic-Ray Ionization." Astrophysical Journal 909, no. 2 (2021): 107. http://dx.doi.org/10.3847/1538-4357/abdc27.

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5

Wittor, Denis. "Cosmic-Ray Acceleration and Magnetic Fields in Galaxy Clusters and Beyond: Insights from Radio Observations." Universe 9, no. 7 (2023): 319. http://dx.doi.org/10.3390/universe9070319.

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The discovery of diffuse radio emission in galaxy clusters proved the existence of energetic cosmic-ray electrons and cosmic magnetic fields on Mpc-scales in the Universe. Furthermore, both magnetic fields and cosmic-ray electrons are predicted to exist beyond galaxy clusters, namely, in the filaments and voids of the cosmic web. Recent detection of diffuse radio emission in intercluster bridges—the region between two merging clusters—strengthens the theory that both cosmic magnetic fields and cosmic-ray electrons exist on these large scales. Radio observations are our most powerful tool to st

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6

Wentzel, Donat G. "Self-Confined Cosmic Rays." Symposium - International Astronomical Union 107 (1985): 341–54. http://dx.doi.org/10.1017/s007418090007580x.

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Cosmic rays do not stream freely through the galaxy, contrary to earlier expectations. Streaming cosmic rays are slowed down by the emission of resonant Alfven waves that scatter the cosmic rays. The theory of self-confinement explains the isotropy of the bulk of the cosmic rays but not of cosmic rays above 103 Gev; it has been a stimulus to the theory for cosmic-ray acceleration at supernova shocks; and, on inclusion of diffusion in a galactic wind, it may explain the uniform cosmic-ray density out to 18 kpc in our galaxy. Rapidly streaming electrons in clusters of galaxies, in supernova remn

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7

KUSENKO, ALEXANDER. "COSMIC CONNECTIONS: FROM COSMIC RAYS TO GAMMA RAYS, COSMIC BACKGROUNDS AND MAGNETIC FIELDS." Modern Physics Letters A 28, no. 02 (2013): 1340001. http://dx.doi.org/10.1142/s0217732313400014.

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Combined data from gamma-ray telescopes and cosmic-ray detectors have produced some new surprising insights regarding intergalactic and galactic magnetic fields, as well as extragalactic background light. We review some recent advances, including a theory explaining the hard spectra of distant blazars and the measurements of intergalactic magnetic fields based on the spectra of distant sources. Furthermore, we discuss the possible contribution of transient galactic sources, such as past gamma-ray bursts and hypernova explosions in the Milky Way, to the observed flux of ultrahigh-energy cosmic-

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Krennrich, Frank. "TeV GAMMA RAYS: OBSERVATIONS VERSUS EXPECTATIONS & THEORY." Acta Polytechnica 53, A (2013): 635–40. http://dx.doi.org/10.14311/ap.2013.53.0635.

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The scope of this paper is to discuss two important questions relevant for TeV γ-ray astronomy; the pursuit to reveal the origin of cosmic rays in our galaxy, and the opacity of the universe in γ-rays. The origin of cosmic rays stipulated the field of TeV astronomy in the first place, and led to the development of the atmospheric Cherenkov technique; significant progress has been made in the last decade through the detection of several supernova remnants, the primary suspects for harboring the acceleration sites of cosmic rays. TeV γ-rays propagate mostly unhindered through the galactic plane,

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9

Shalchi, A. "Second-order quasilinear theory of cosmic ray transport." Physics of Plasmas 12, no. 5 (2005): 052905. http://dx.doi.org/10.1063/1.1895805.

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10

Starodubtsev, Sergei. "Shape of spectrum of galactic cosmic ray intensity fluctuations." Solar-Terrestrial Physics 8, no. 2 (2022): 71–75. http://dx.doi.org/10.12737/stp-82202211.

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The impact of solar wind plasma on fluxes of galactic cosmic rays (CR) penetrating from the outside into the heliosphere with energies above ~1 GeV leads to temporal variations in the CR intensity in a wide frequency range. Cosmic rays being charged particles, their modulation occurs mainly under impacts of the interplanetary magnetic field. It is well known that the observed spectrum of interplanetary magnetic field (IMF) fluctuations in a wide frequency range ν from ~10–7 to ~10 Hz has a pronounced falling character and consists of three sections: energy, inertial, and dissipative. Eac

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11

Schlickeiser, Reinhard. "Cosmic-Ray Transport and Acceleration." International Astronomical Union Colloquium 142 (1994): 926–36. http://dx.doi.org/10.1017/s0252921100078337.

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AbstractWe review the transport and acceleration of cosmic rays concentrating on the origin of galactic cosmic rays. Quasi-linear theory for the acceleration rates and propagation parameters of charged test particles combined with the plasma wave viewpoint of modeling weak cosmic electromagnetic turbulence provides a qualitatively and quantitatively correct description of key observations. Incorporating finite frequency effects, dispersion, and damping of the plasma waves are essential in overcoming classical discrepancies with observations as the Kfit - Kql discrepancy of solar particle event

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12

Heintz, Evan, and Ellen G. Zweibel. "Galaxies at a Cosmic Ray Eddington Limit." Astrophysical Journal 941, no. 1 (2022): 78. http://dx.doi.org/10.3847/1538-4357/ac9e9e.

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Abstract Cosmic rays have been shown to be extremely important in the dynamics of diffuse gas in galaxies, helping to maintain hydrostatic equilibrium, and serving as a regulating force in star formation. In this paper, we address the influence of cosmic rays on galaxies by re-examining the theory of a cosmic ray Eddington limit, first proposed by Socrates et al. and elaborated upon by Crocker et al. and Huang & Davis. A cosmic ray Eddington limit represents a maximum cosmic ray energy density above which the interstellar gas cannot be in hydrostatic equilibrium, resulting in a wind. In th

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13

Zank, G. P. "A cosmic-ray-driven plasma instability." Journal of Plasma Physics 41, no. 1 (1989): 89–95. http://dx.doi.org/10.1017/s0022377800013684.

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The stability of the MHD equations describing the mutual interaction of cosmic rays, thermal plasma, magnetic field and Alfvén waves used in cosmic-ray-shock acceleration theory (e.g. McKenzie & Völk 1982) is analysed for linear compressive instabilities. It is found that the inclusion of wave effects implies that the forward propagating sub-Alfvénic mode is unstable on wavelength scales greater than 1 parsec. The role of the instability in astrophysical models is considered.

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14

Petrov, Nikolay, Nikolay Goutev, Hristo Protohristov, Dimitar Tonev, and Galina Dimitrova. "PORTABLE MUON TELESCOPE FOR COSMIC RAY MONITORING." Ecological Engineering and Environment Protection 2024, no. 1/2024 (2024): 43–46. http://dx.doi.org/10.32006/eeep.2024.1.4346.

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A portable muon telescope for monitoring of cosmic rays has been developed, based on GM counters shielded with lead adsorbers. The triple coincidence mode of operation results in a relatively good spatial resolution allowing to measure the cosmic ray flux, its east-west anomaly and also to detect the consequences of the special theory of relativity. The apparatus is suitable for long term observations of the cosmic ray flux and due to its simple and robust construction can also be used also for educational purposes.

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15

Tatischeff, Vincent, and Stefano Gabici. "Particle Acceleration by Supernova Shocks and Spallogenic Nucleosynthesis of Light Elements." Annual Review of Nuclear and Particle Science 68, no. 1 (2018): 377–404. http://dx.doi.org/10.1146/annurev-nucl-101917-021151.

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In this review, we first reassess the supernova remnant paradigm for the origin of Galactic cosmic rays in the light of recent cosmic-ray data acquired by the Voyager 1 spacecraft. We then describe the theory of light-element nucleosynthesis by nuclear interaction of cosmic rays with the interstellar medium and outline the problem of explaining the measured beryllium abundances in old halo stars of low metallicity with the standard model of the Galactic cosmic-ray origin. We then discuss the various cosmic-ray models proposed in the literature to account for the measured evolution of the light

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16

Mertsch, P., and M. Ahlers. "Cosmic ray small-scale anisotropies in quasi-linear theory." Journal of Cosmology and Astroparticle Physics 2019, no. 11 (2019): 048. http://dx.doi.org/10.1088/1475-7516/2019/11/048.

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17

Zhang, Ming. "A Markov Stochastic Process Theory of Cosmic‐Ray Modulation." Astrophysical Journal 513, no. 1 (1999): 409–20. http://dx.doi.org/10.1086/306857.

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18

Munakata, K., and K. Nagashima. "A theory of cosmic ray anisotropies of solar origin." Planetary and Space Science 34, no. 1 (1986): 99–116. http://dx.doi.org/10.1016/0032-0633(86)90107-8.

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19

Thielheim, K. O. "Cosmic Ray Particle Acceleration in Pulsar Magnetospheres." Symposium - International Astronomical Union 125 (1987): 555. http://dx.doi.org/10.1017/s0074180900161406.

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A plausible approach to the theory of pulsars as cosmic ray particle accelerators is to integrate numerically the Lorentz-Dirac-equation, using the vacuum field of a rotating orthogonal magnetic dipole as a model field configuration. Typical parameter values are: angular velocity ω = 20 π/sec and magnetic dipole moment μ = 1030G cm3 (K.O. Thielheim, Proc. ESO-CERN Conf. 1986).

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20

Kálosi, Ábel, Lisa Gamer, Manfred Grieser, et al. "Dissociative Recombination of Rotationally Cold OH⁺ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds." Astrophysical Journal Letters 955, no. 2 (2023): L26. http://dx.doi.org/10.3847/2041-8213/acf71d.

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Abstract Observations of OH+ are used to infer the interstellar cosmic ray ionization rate in diffuse atomic clouds, thereby constraining the propagation of cosmic rays through and the shielding by interstellar clouds, as well as the low energy cosmic ray spectrum. In regions where the H2-to-H number density ratio is low, dissociative recombination (DR) is the dominant destruction process for OH+ and the DR rate coefficient is important for predicting the OH+ abundance and inferring the cosmic ray ionization rate. We have experimentally studied DR of electronically and vibrationally relaxed OH

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21

Wittor, D., F. Vazza, D. Ryu, and H. Kang. "Limiting the shock acceleration of cosmic ray protons in the ICM." Monthly Notices of the Royal Astronomical Society: Letters 495, no. 1 (2020): L112—L117. http://dx.doi.org/10.1093/mnrasl/slaa066.

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ABSTRACT Observations of large-scale radio emissions prove the existence of shock accelerated cosmic ray electrons in galaxy clusters, while the lack of detected γ-rays limits the acceleration of cosmic ray protons in galaxy clusters. This challenges our understanding of how diffusive shock acceleration works. In this work, we couple the most updated recipes for shock acceleration in the intracluster medium to state-of-the-art magnetohydrodynamical simulations of massive galaxy clusters. Furthermore, we use passive tracer particles to follow the evolution of accelerated cosmic rays. We show th

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22

Wandel, Amri. "Supernova Remnants and the ISM: Constraints from Cosmic-Ray Acceleration." International Astronomical Union Colloquium 101 (1988): 325–29. http://dx.doi.org/10.1017/s0252921100102581.

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AbstractSupernova remnants can reaccelerate cosmic rays and modify their distribution during the cosmic ray propagation in the galaxy. Cosmic ray observations (in particular the boron-to-carbon data) strongly limit the permitted amount of reacceleration, which is used to set an upper limit on the expansion of supernova remnants, and a lower limit on the effective density of the ISM swept up by supernova shocks. The constraint depends on the theory of cosmic ray propagation: the standard Leaky Box model requires a high effective density, > 1cm−3, and is probably inconsistent with the present

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23

Tjus, Julia Becker. "Plasmas, particles and photons—spotlights on multimessenger astronomy." Plasma Physics and Controlled Fusion 64, no. 4 (2022): 044013. http://dx.doi.org/10.1088/1361-6587/ac57ce.

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Abstract During the past decennia, progress in the area of high-energy astroparticle physics was exceptional, mainly due to the great success of the bridging of particle- and astrophysics both in theory and in the instrumentation of astroparticle physics observatories. Multimessenger data coming from charged cosmic-ray-, gamma-ray- and neutrino-observatories start to shed more and more light on the nature and origin of cosmic rays. At the same time, the development of methods for the investigation of cosmic-ray transport, acceleration and interaction has advanced to the true potential of tying

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24

BLARD, P., D. BOURLES, J. LAVE, and R. PIK. "Applications of ancient cosmic-ray exposures: Theory, techniques and limitations." Quaternary Geochronology 1, no. 1 (2006): 59–73. http://dx.doi.org/10.1016/j.quageo.2006.06.003.

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25

Caprioli, Damiano. "Cosmic-ray acceleration in supernova remnants: non-linear theory revised." Journal of Cosmology and Astroparticle Physics 2012, no. 07 (2012): 038. http://dx.doi.org/10.1088/1475-7516/2012/07/038.

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26

Fornieri, Ottavio, Daniele Gaggero, Silvio Sergio Cerri, Pedro De La Torre Luque, and Stefano Gabici. "The theory of cosmic ray scattering on pre-existing MHD modes meets data." Monthly Notices of the Royal Astronomical Society 502, no. 4 (2021): 5821–38. http://dx.doi.org/10.1093/mnras/stab355.

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ABSTRACT We present a comprehensive study about the phenomenological implications of the theory describing Galactic cosmic ray scattering on to magnetosonic and Alfvénic fluctuations in the GeV−PeV domain. We compute a set of diffusion coefficients from first principles, for different values of the Alfvénic Mach number and other relevant parameters associated with both the Galactic halo and the extended disc, taking into account the different damping mechanisms of turbulent fluctuations acting in these environments. We confirm that the scattering rate associated with Alfvénic turbulence is hig

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27

Reichherzer, P., J. Becker Tjus, E. G. Zweibel, L. Merten, and M. J. Pueschel. "Turbulence-level dependence of cosmic ray parallel diffusion." Monthly Notices of the Royal Astronomical Society 498, no. 4 (2020): 5051–64. http://dx.doi.org/10.1093/mnras/staa2533.

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ABSTRACT Understanding the transport of energetic cosmic rays belongs to the most challenging topics in astrophysics. Diffusion due to scattering by electromagnetic fluctuations is a key process in cosmic ray transport. The transition from a ballistic to a diffusive-propagation regime is presented in direct numerical calculations of diffusion coefficients for homogeneous magnetic field lines subject to turbulent perturbations. Simulation results are compared with theoretical derivations of the parallel diffusion coefficient’s dependences on the energy and the fluctuation amplitudes in the limi

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28

Dorfi, E. A. "Evolution of Supernova Remnants with Cosmic Rays and Radiative Cooling." International Astronomical Union Colloquium 142 (1994): 841–44. http://dx.doi.org/10.1017/s0252921100078192.

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AbstractRecent numerical models for SNR evolution are presented, including first-order Fermi acceleration with injection of suprathermal particles at the shock wave, heating due to dissipation of Alfvén waves in the precursor region and radiative cooling of the thermal plasma. The X-ray fluxes obtained from these SNR models show significant differences depending on the acceleration efficiency of cosmic rays. γ-ray fluxes are calculated originating from π0-decay of pions generated by collisions of the high-energy particles with the thermal plasma. Cooling of the thermal plasma and dissipation o

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Uchaikin, Vladimir V., Ilya I. Kozhemyakin, and Vladimir A. Litvinov. "On the classical approach to describing the diffusion of cosmic rays in a turbulent medium." Âdernaâ fizika 87, no. 2 (2024): 96–101. http://dx.doi.org/10.31857/s0044002724020053.

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The inhomogeneous structure of the interstellar medium (ISM) is characterized by largescale fluctuations that significantly affect the cosmic ray propagation process. Accounting for this influence can not only lead to adjustments in the diffusion process parameters but even to pass from differential operators to integral ones. The most crucial characteristics of a turbulent medium is its power spectrum. Including appropriate approximations of this spectrum allows us to consider this problem in the framework of the traditional diffusion approach [1, 2]. This article explores the analytical repr

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Wibig, Tadeusz, and Arnold W. Wolfendale. "Cosmic ray contributions to the WMAP polarization data on the cosmic microwave background." International Journal of Modern Physics D 25, no. 03 (2016): 1650029. http://dx.doi.org/10.1142/s0218271816500292.

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We have updated our analysis of the 9-year WMAP data using the collection of polarization maps looking for the presence of additional evidence for a finite ‘cosmic ray (CR) foreground’ for the cosmic microwave background (CMB). We have given special attention to high Galactic latitudes, where the recent BICEP2 findings were reported although very recent Planck data claims that dust is prevalent, thus nullifying the BICEP2 results. The method of examining the correlation with the observed gamma ray flux proposed in our earlier papers and applied to the polarization data shows that the foregroun

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31

Mesinger, Andrei. "Reionization and Cosmic Dawn: theory and simulations." Proceedings of the International Astronomical Union 12, S333 (2017): 3–11. http://dx.doi.org/10.1017/s1743921317011139.

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AbstractWe highlight recent progress in the sophistication and diversification of the simulations of cosmic dawn and reionization. The application of these modeling tools to recent observations has allowed us narrow down the timing of reionization. The midpoint of reionization is constrained to z = 7.6−0.7+0.8 (1 σ), with the strongest constraints coming from the optical depth to the CMB measured with the Planck satellite and the first detection of ongoing reionization from the spectra of the z = 7.1 QSOs ULASJ1120+0641. However, we still know virtually nothing about the astrophysical sources

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32

Plebaniak, Zbigniew, and Tadeusz Wibig. "EAS longitudinal development distribution parameters for different extrapolations of the nuclei intaraction cross section to the very high energy domain." EPJ Web of Conferences 208 (2019): 08016. http://dx.doi.org/10.1051/epjconf/201920808016.

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Determination of the primary particle mass using air fluorescence or a Cherenkov detector array is one of the most difficult task of experimental cosmic ray studies. The information about the primary particle mass is a compound of the produced particle multiplicity, inelasticity, interaction cross-section and many other parameters, thus it is necessary to compare registered showers with sophisticated Monte-Carlo simulation results. In this work we present results of the studies of at least three possible ways of extrapolating proton- Nucleus and Nucleus-Nucleus cross sections to cosmic ray ene

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33

HESS, PETER O., and WALTER GREINER. "PSEUDO-COMPLEX FIELD THEORY." International Journal of Modern Physics E 16, no. 06 (2007): 1643–79. http://dx.doi.org/10.1142/s0218301307006964.

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A new formulation of field theory is presented, based on a pseudo-complex description. An extended group structure is introduced, implying a minimal scalar length, rendering the theory regularized a la Pauli–Villars. Cross sections are calculated for the scattering of an electron at an external Coulomb field and the Compton scattering. Deviations due to a smallest scalar length are determined. The theory also permits a modification of the minimal coupling scheme, resulting in a generalized dispersion relation. A shift of the Greisen–Zatsepin–Kuzmin (GZK) limit of the cosmic ray spectrum is the

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34

Huege, T. "Simulations and theory of radio emission from cosmic ray air showers." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 604, no. 1-2 (2009): S57—S63. http://dx.doi.org/10.1016/j.nima.2009.03.165.

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35

Schlickeiser, Reinhard, and Ulrich Achatz. "Cosmic-ray particle transport in weakly turbulent plasmas. Part 1. Theory." Journal of Plasma Physics 49, no. 1 (1993): 63–77. http://dx.doi.org/10.1017/s0022377800016822.

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We consider a quasi-linear theory for the acceleration rates and propagation parameters of charged test particles in weakly turbulent electromagnetic plasmas. The similarity between two recent approaches to modelling of therandom electromagnetic field is demonstrated. It is shown that both the concept of dynamical magnetic turbulence and the concept of superposition of individual plasma modes lead to particle Fokker—Planck coefficients in which the sharp delta functions describing the resonant interaction of the particles have to be replaced by Breit—Wigner-type resonance functions, which are

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36

Blandford, Roger, and David Eichler. "Particle acceleration at astrophysical shocks: A theory of cosmic ray origin." Physics Reports 154, no. 1 (1987): 1–75. http://dx.doi.org/10.1016/0370-1573(87)90134-7.

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37

Busoni, Giorgio, and Laura Prati. "Theory of Evolution Systems Applied to a Cosmic Ray Diffusion Model." Transport Theory and Statistical Physics 40, no. 1 (2011): 23–67. http://dx.doi.org/10.1080/00411450.2011.563813.

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38

Burde, Georgy I. "Lorentz Violation by the Preferred Frame Effects and Cosmic and Gamma Ray Propagation." Galaxies 9, no. 4 (2021): 119. http://dx.doi.org/10.3390/galaxies9040119.

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The ‘relativity with a preferred frame’, designed to reconcile the relativity principle with the existence of the cosmological preferred frame, incorporates the preferred frame at the level of special relativity (SR) while retaining the fundamental spacetime symmetry, which, in the standard SR, manifests itself as Lorentz invariance. In this paper, the processes, accompanying the propagation of cosmic rays and gamma rays through the background radiation from distant sources to Earth, are considered on the basis of particle dynamics and electromagnetic field dynamics developed within the framew

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Berezhko, E. G., G. Pühlhofer та H. J. Völk. "Theory of cosmic ray and γ-ray production in the supernova remnant RX J0852.0-4622". Astronomy & Astrophysics 505, № 2 (2009): 641–54. http://dx.doi.org/10.1051/0004-6361/200809473.

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40

Starodubtsev, Sergei. "Shape of spectrum of galactic cosmic ray intensity fluctuations." Solnechno-Zemnaya Fizika 8, no. 2 (2022): 78–83. http://dx.doi.org/10.12737/szf-82202211.

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The impact of solar wind plasma on fluxes of galactic cosmic rays (CR) penetrating from the outside into the heliosphere with energies above ~1 GeV leads to temporal variations in the CR intensity in a wide frequency range. Cosmic rays being charged particles, their modulation occurs mainly under impacts of the interplanetary magnetic field. It is well known that the observed spectrum of interplanetary magnetic field (IMF) fluctuations in a wide frequency range ν from ~10–7 to ~10 Hz has a pronounced falling character and consists of three sections: energy, inertial, and dissipative. Eac

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41

Stepanov, Rodion, A. Fletcher, A. Shukurov, R. Beck, L. La Porta, and F. S. Tabatabaei. "Relative distributions of cosmic ray electrons and magnetic fields in the ISM." Proceedings of the International Astronomical Union 4, S259 (2008): 93–94. http://dx.doi.org/10.1017/s1743921309030130.

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AbstractWe calculate the relative magnitudes of the fluctuations in total synchrotron intensity in the interstellar medium, both from observations and from theory under various assumptions about the correlation or anticorrelation between cosmic rays and interstellar magnetic fields. The results are inconsistent with local energy equipartition between cosmic rays and magnetic fields. The distribution of cosmic rays must be rather uniform at scales of order 1 kpc, whereas interstellar magnetic fields vary at much smaller scales.

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Biermann, Peter L., Philipp P. Kronberg, Michael L. Allen, Athina Meli, and Eun-Suk Seo. "The Origin of the Most Energetic Galactic Cosmic Rays: Supernova Explosions into Massive Star Plasma Winds." Galaxies 7, no. 2 (2019): 48. http://dx.doi.org/10.3390/galaxies7020048.

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We propose that the high energy Cosmic Ray particles up to the upturn commonly called the ankle, from around the spectral turn-down commonly called the knee, mostly come from Blue Supergiant star explosions. At the upturn, i.e., the ankle, Cosmic Rays probably switch to another source class, most likely extragalactic sources. To show this we recently compiled a set of Radio Supernova data where we compute the magnetic field, shock speed and shock radius. This list included both Blue and Red Supergiant star explosions; both data show the same magnetic field strength for these two classes of sta

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CHEN, SHAO-XIA, and ZHAO-YU YANG. "NONCOMMUTATIVITY AS A POSSIBLE ORIGIN OF THE ULTRAHIGH ENERGY COSMIC RAY AND THE TeV-PHOTON PARADOXES." Modern Physics Letters A 18, no. 40 (2003): 2913–19. http://dx.doi.org/10.1142/s0217732303012398.

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In this paper, we present a general modified dispersion relation derived from q-deformed noncommutative theory and apply it to the ultrahigh energy cosmic ray and the TeV-photon paradoxes — threshold anomalies. Our purpose is not only trying to solve these puzzles by noncommutative theory but also to support noncommutative theory through the coincidence of the region in the parameter space for resolving the threshold anomalies with the one from the q-deformed noncommutative theory.

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AMELINO-CAMELIA, GIOVANNI. "KINEMATICAL SOLUTION OF THE UHE-COSMIC-RAY PUZZLE WITHOUT A PREFERRED CLASS OF INERTIAL OBSERVERS." International Journal of Modern Physics D 12, no. 07 (2003): 1211–26. http://dx.doi.org/10.1142/s0218271803003645.

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Among the possible explanations for the puzzling observations of cosmic rays above the GZK cutoff there is growing interest in the ones that represent kinematical solutions, based either on general formulations of particle physics with small violations of Lorentz symmetry or on a quantum-gravity-motivated scheme for the breakdown of Lorentz symmetry. An unappealing aspect of these cosmic-ray-puzzle solutions is that they require the existence of a preferred class of inertial observers. Here I propose a new kinematical solution of the cosmic-ray puzzle, which does not require the existence of a

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Shapiro, V. D., K. B. Quest, and M. Okolicsanyi. "Non-resonant firehose instability: Consequences for the theory of cosmic ray acceleration." Geophysical Research Letters 25, no. 6 (1998): 845–48. http://dx.doi.org/10.1029/98gl00467.

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Berezhko, E. G., and H. J. Völk. "Theory of cosmic ray production in the supernova remnant RX J1713.7-3946." Astronomy & Astrophysics 451, no. 3 (2006): 981–90. http://dx.doi.org/10.1051/0004-6361:20054595.

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Ellison, Donald C., and David Eichler. "Relativistic Cosmic-Ray Spectra in the Fully Nonlinear Theory of Shock Acceleration." Physical Review Letters 55, no. 24 (1985): 2735–38. http://dx.doi.org/10.1103/physrevlett.55.2735.

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Hussein, M., and A. Shalchi. "DETAILED NUMERICAL INVESTIGATION OF THE BOHM LIMIT IN COSMIC RAY DIFFUSION THEORY." Astrophysical Journal 785, no. 1 (2014): 31. http://dx.doi.org/10.1088/0004-637x/785/1/31.

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Zhang, Ming. "A Path Integral Approach to the Theory of Heliospheric Cosmic‐Ray Modulation." Astrophysical Journal 510, no. 2 (1999): 715–25. http://dx.doi.org/10.1086/306624.

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Fiorillo, Damiano F. G., Luca Comisso, Enrico Peretti, Maria Petropoulou, and Lorenzo Sironi. "A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068." Astrophysical Journal 974, no. 1 (2024): 75. http://dx.doi.org/10.3847/1538-4357/ad7021.

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Abstract:

Abstract The cores of active galactic nuclei are potential accelerators of 10–100 TeV cosmic rays, in turn producing high-energy neutrinos. This picture was confirmed by the compelling evidence of a TeV neutrino signal from the nearby active galaxy NGC 1068, leaving open the question of what is the site and mechanism of cosmic-ray acceleration. One candidate is the magnetized turbulence surrounding the central supermassive black hole. Recent particle-in-cell simulations of magnetized turbulence indicate that stochastic cosmic-ray acceleration is nonresonant, in contrast to the assumptions of p

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